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"/tmp/binary_c_python-dh00601/failed_systems", "_population_id": "3c147f14b9a74e3b8aedebcd04d0265c", "_total_mass_run": 0, "_total_probability_weighted_mass_run": 0, "modulo": 1, "start_at": 0, "skip_before": 0, "_sampling_variables": {"multiplicity": {"name": "multiplicity", "parameter_name": "multiplicity", "longname": "multiplicity", "valuerange": [1, 2], "samplerfunc": "self.const_int(1, 2, 2)", "precode": "self.population_options[\"multiplicity\"] = multiplicity; self.bse_options[\"multiplicity\"] = multiplicity; options={'q_high_extrapolation_method': 'flat', 'Mmin': 0.08, 'samplerfuncs': {'M': [None, None, None, None], 'logP': [None, None, None], 'ecc': [None, None, None]}, 'IMF_distribution': 'kroupa2001', 'JSON': None, 'q_low_extrapolation_method': 'flat', 'multiplicity_model': 'Poisson', 'normalize_multiplicities': 'merge', 'setup grid': True, 'clean load flag': False, 'apply settings': True, 'clean cache': False, 'load data': True, 'clean all': False, 'ranges': {'q': [None, None], 'ecc': [0.0, 0.99], 'M': [0.084, 120], 'logP': [0.0, 8.0]}, 'resolutions': {'ecc': [0, 0, 0], 'M': [80, 80, 0, 0], 'logP': [80, 0, 0]}, 'multiplicity_modulator': [0, 1, 0, 0]}", "postcode": null, "probdist": 1, "dphasevol": -1, "condition": "([0, 1, 0, 0][int(multiplicity)-1] > 0)", "gridtype": "discrete", "branchpoint": 0, "branchcode": null, "topcode": null, "bottomcode": null, "sampling_variable_number": 0, "dry_parallel": false, "dependency_variables": null}, "lnM_1": {"name": "lnM_1", "parameter_name": "M_1", "longname": "Primary mass", "valuerange": ["np.log(0.084)", "np.log(120)"], "samplerfunc": "self.const_linear(np.log(0.084), np.log(120), 80)", "precode": "M_1 = np.exp(lnM_1); options[\"M_1\"]=M_1", "postcode": null, "probdist": "self.Moe_di_Stefano_2017_pdf({'q_high_extrapolation_method': 'flat', 'Mmin': 0.08, 'samplerfuncs': {'M': [None, None, None, None], 'logP': [None, None, None], 'ecc': [None, None, None]}, 'IMF_distribution': 'kroupa2001', 'JSON': None, 'q_low_extrapolation_method': 'flat', 'multiplicity_model': 'Poisson', 'normalize_multiplicities': 'merge', 'setup grid': True, 'clean load flag': False, 'apply settings': True, 'clean cache': False, 'load data': True, 'clean all': False, 'ranges': {'q': [None, None], 'ecc': [0.0, 0.99], 'M': [0.084, 120], 'logP': [0.0, 8.0]}, 'resolutions': {'ecc': [0, 0, 0], 'M': [80, 80, 0, 0], 'logP': [80, 0, 0]}, 'multiplicity_modulator': [0, 1, 0, 0], 'multiplicity': multiplicity, 'M_1': M_1}, verbosity=self.population_options['verbosity'])['total_probdens'] if multiplicity == 1 else 1", "dphasevol": "dlnM_1", "condition": null, "gridtype": "centred", "branchpoint": 1, "branchcode": "multiplicity == 1", "topcode": null, "bottomcode": null, "sampling_variable_number": 1, "dry_parallel": false, "dependency_variables": null}, "log10per": {"name": "log10per", "parameter_name": "orbital_period", "longname": "log10(Orbital_Period)", "valuerange": [0.0, 8.0], "samplerfunc": "self.const_linear(0.0, 8.0, 80)", "precode": "orbital_period = 10.0**log10per\nqmin=0.08/M_1\nqmax=maximum_mass_ratio_for_RLOF(M_1, orbital_period)\n", "postcode": null, "probdist": 1.0, "dphasevol": "(0.43429448190325176 * dlog10per)", "condition": "(self.population_options[\"multiplicity\"] >= 2)", "gridtype": "centred", "branchpoint": 0, "branchcode": null, "topcode": null, "bottomcode": null, "sampling_variable_number": 2, "dry_parallel": false, "dependency_variables": null}, "q": {"name": "q", "parameter_name": "M_2", "longname": "Mass ratio", "valuerange": [null, null], "samplerfunc": "self.const_linear(0.08/M_1, qmax, 80)", "precode": "\nM_2 = q * M_1\nsep = calc_sep_from_period(M_1, M_2, orbital_period)\n    ", "postcode": null, "probdist": "self.Moe_di_Stefano_2017_pdf({'q_high_extrapolation_method': 'flat', 'Mmin': 0.08, 'samplerfuncs': {'M': [None, None, None, None], 'logP': [None, None, None], 'ecc': [None, None, None]}, 'IMF_distribution': 'kroupa2001', 'JSON': None, 'q_low_extrapolation_method': 'flat', 'multiplicity_model': 'Poisson', 'normalize_multiplicities': 'merge', 'setup grid': True, 'clean load flag': False, 'apply settings': True, 'clean cache': False, 'load data': True, 'clean all': False, 'ranges': {'q': [None, None], 'ecc': [0.0, 0.99], 'M': [0.084, 120], 'logP': [0.0, 8.0]}, 'resolutions': {'ecc': [0, 0, 0], 'M': [80, 80, 0, 0], 'logP': [80, 0, 0]}, 'multiplicity_modulator': [0, 1, 0, 0], \"multiplicity\": multiplicity, \"M_1\": M_1, \"M_2\": M_2, \"M_3\": M_3, \"M_4\": M_4, \"P\": orbital_period, \"P2\": orbital_period_triple, \"P3\": orbital_period_quadruple, \"ecc\": eccentricity, \"ecc2\": eccentricity_triple, \"ecc3\": eccentricity_quadruple}, verbosity=self.population_options['verbosity'])['total_probdens']", "dphasevol": "dq", "condition": null, "gridtype": "centred", "branchpoint": 0, "branchcode": null, "topcode": null, "bottomcode": null, "sampling_variable_number": 3, "dry_parallel": false, "dependency_variables": null}}, "gridcode_filename": "/vol/ph/astro_data/dhendriks/binary_c_results/RLOF/EVENTS_V2.2.4_HIGH_RES_EXPLORATION_BALLISTIC_RLOF_2021_MOE_DISTEFANO/population_results/Z0.02/local_tmp_dir/binary_c_grid_3c147f14b9a74e3b8aedebcd04d0265c.py", "symlink_latest_gridcode": true, "save_population_object": null, "joinlist": null, "do_analytics": true, "save_snapshots": false, "save_snapshot": false, "restore_from_snapshot_file": null, "restore_from_snapshot_dir": null, "exit_code": 0, "stop_queue": false, "_killed": false, "_queue_done": true, "monte_carlo_count_threshold": -1, "_monte_carlo_current_total_count_evolved": 0, "monte_carlo_mass_threshold": -1, "_monte_carlo_current_total_mass_evolved": 0, "monte_carlo_custom_threshold_function": null, "_monte_carlo_threshold_reached": false, "_monte_carlo_generator_filename": null, "monte_carlo_use_pre_calculated_distributions": true, "source_file_sampling_filename": null, "source_file_sampling_type": "commands", "_source_file_filehandle": null, "custom_generator": null, "function_cache": true, "function_cache_default_maxsize": 256, "function_cache_default_type": "NullCache", "function_cache_TTL": 30, "function_cache_functions": {"distribution_functions.powerlaw_constant": [0, "NoCache", "1,100,-2"], "distribution_functions.calculate_constants_three_part_powerlaw": [16, "FIFOCache", "0.1,0.5,1,100,-1.3,-2.3,-2.3"], "distribution_functions.gaussian_normalizing_const": [16, "FIFOCache", "1.0,1.0,-10.0,+10.0"], "spacing_functions.const_linear": [16, "FIFOCache", "1,10,9"], "spacing_functions.const_int": [0, null, "1,10,9"], "spacing_functions.const_ranges": [16, "FIFOCache", "((0.1,0.65,10),(0.65,0.85,20),(0.85,10.0,10))"], "spacing_functions.gaussian_zoom": [16, "FIFOCache", "1.0,10.0,5.0,2.0,0.9,100"]}, "HPC_force_join": 0, "HPC_rebuild_joinlist": 0, "slurm": 0, "slurm_ntasks": 1, "slurm_dir": "", "slurm_jobid": "", "slurm_memory": "512MB", "slurm_warn_max_memory": "1024MB", "slurm_postpone_join": 0, "slurm_jobarrayindex": null, "slurm_jobname": "binary_c-python", "slurm_partition": null, "slurm_time": "0", "slurm_postpone_sbatch": 0, "slurm_array": null, "slurm_array_max_jobs": null, "slurm_extra_settings": {}, "slurm_sbatch": null, "slurm_env": "/usr/bin/env", "slurm_bash": "/usr/local/bin/bash", "slurm_pwd": "/bin/pwd", "slurm_date": "/bin/date", "condor": 0, "condor_dir": "", "condor_njobs": 0, "condor_ClusterID": null, "condor_Process": null, "condor_postpone_submit": 0, "condor_postpone_join": 0, "condor_memory": 512, "condor_warn_max_memory": 1024, "condor_universe": "vanilla", "condor_extra_settings": {}, "condor_snapshot_on_kill": 0, "condor_stream_output": true, "condor_stream_error": true, "condor_should_transfer_files": "YES", "condor_when_to_transfer_output": "ON_EXIT_OR_EVICT", "condor_requirements": "", "condor_env": "/usr/bin/env", "condor_bash": "/usr/local/bin/bash", "condor_pwd": "/bin/pwd", "condor_date": "/bin/date", "condor_initial_dir": null, "condor_submit": null, "condor_q": null, "condor_getenv": true, "condor_batchname": "binary_c-condor", "condor_kill_sig": "SIGINT", "event_based_logging_handle_output": false, "event_based_logging_output_directory": "/vol/ph/astro_data/dhendriks/binary_c_results/RLOF/EVENTS_V2.2.4_HIGH_RES_EXPLORATION_BALLISTIC_RLOF_2021_MOE_DISTEFANO/population_results/Z0.02/events", "event_based_logging_combine_individual_event_files": false, "event_based_logging_combined_events_filename": "all_events.dat", "event_based_logging_remove_individual_event_files_after_combining": false, "event_based_logging_split_events_file_to_each_type": false, "event_based_logging_remove_original_combined_events_file_after_splitting": false, "event_based_logging_output_separator": "\t", "event_based_logging_output_parser": "<function event_based_logging_output_parser at 0x2b7188e7cb80>", "event_based_logging_parameter_list_dict": {"SN_BINARY": ["uuid", "probability", "event_number", "event_type", "zams_mass_1", "zams_mass_2", "zams_orbital_period", "zams_separation", "zams_eccentricity", "time", "metallicity", "random_seed", "SN_post_SN_mass", "SN_post_SN_stellar_type", "SN_type", "SN_fallback_fraction", "SN_fallback_mass", "SN_post_SN_ecc", "SN_post_SN_orbital_period", "SN_post_SN_separation", "SN_pre_SN_mass", "SN_pre_SN_stellar_type", "SN_pre_SN_radius", "SN_pre_SN_core_mass", "SN_pre_SN_CO_core_mass", "SN_pre_SN_He_core_mass", "SN_pre_SN_fraction_omega_crit", "SN_pre_SN_ecc", "SN_pre_SN_orbital_period", "SN_pre_SN_separation", "SN_pre_SN_companion_mass", "SN_pre_SN_companion_radius", "SN_pre_SN_companion_stellar_type", "SN_starnum", "SN_counter", "SN_kick_v", "SN_kick_omega", "SN_kick_phi"], "SN_SINGLE": ["uuid", "probability", "event_number", "event_type", "zams_mass_1", "time", "metallicity", "random_seed", "SN_post_SN_mass", "SN_post_SN_stellar_type", "SN_type", "SN_fallback_fraction", "SN_fallback_mass", "SN_pre_SN_mass", "SN_pre_SN_stellar_type", "SN_pre_SN_radius", "SN_pre_SN_core_mass", "SN_pre_SN_CO_core_mass", "SN_pre_SN_He_core_mass", "SN_pre_SN_fraction_omega_crit", "SN_starnum", "SN_counter", "SN_kick_v", "SN_kick_omega", "SN_kick_phi"], "RLOF": ["uuid", "probability", "event_number", "event_type", "zams_mass_1", "zams_mass_2", "zams_orbital_period", "zams_separation", "zams_eccentricity", "time", "metallicity", "random_seed", "RLOF_initial_mass_accretor", "RLOF_initial_mass_donor", "RLOF_initial_radius_accretor", "RLOF_initial_radius_donor", "RLOF_initial_separation", "RLOF_initial_orbital_period", "RLOF_initial_stellar_type_accretor", "RLOF_initial_stellar_type_donor", "RLOF_initial_orbital_angular_momentum", "RLOF_initial_stability", "RLOF_initial_starnum_accretor", "RLOF_initial_starnum_donor", "RLOF_initial_time", "RLOF_initial_disk", "RLOF_final_mass_accretor", "RLOF_final_mass_donor", "RLOF_final_radius_accretor", "RLOF_final_radius_donor", "RLOF_final_separation", "RLOF_final_orbital_period", "RLOF_final_stellar_type_accretor", "RLOF_final_stellar_type_donor", "RLOF_final_orbital_angular_momentum", "RLOF_final_stability", "RLOF_final_starnum_accretor", "RLOF_final_starnum_donor", "RLOF_final_time", "RLOF_final_disk", "RLOF_total_mass_lost", "RLOF_total_mass_lost_from_accretor", "RLOF_total_mass_lost_from_disk", "RLOF_total_mass_lost_from_common_envelope", "RLOF_total_mass_accreted", "RLOF_total_mass_transferred", "RLOF_total_time_spent_masstransfer", "RLOF_total_orbital_angular_momentum_lost_through_mass_loss_from_star", "RLOF_total_orbital_angular_momentum_lost_through_mass_loss_from_disk", "RLOF_total_orbital_angular_momentum_lost_through_mass_loss", "RLOF_total_orbital_angular_momentum_stream_excess_returned_to_orbit", "RLOF_total_orbital_angular_momentum_stellar_overspin_returned_to_orbit", "RLOF_total_orbital_angular_momentum_stream_torque_with_orbit_gain", "RLOF_total_orbital_angular_momentum_stream_torque_with_orbit_loss", "RLOF_total_mass_transferred_through_disk", "RLOF_total_mass_transferred_through_disk_CATEGORY_COLD", "RLOF_total_mass_transferred_through_disk_CATEGORY_UNSTABLE", "RLOF_total_mass_transferred_through_disk_CATEGORY_HOT", "RLOF_total_mass_transferred_through_disk_CATEGORY_PARTIALLY_THICK", "RLOF_total_mass_transferred_through_disk_CATEGORY_THICK", "RLOF_total_time_spent_disk_masstransfer", "RLOF_total_time_spent_disk_masstransfer_CATEGORY_COLD", "RLOF_total_time_spent_disk_masstransfer_CATEGORY_UNSTABLE", "RLOF_total_time_spent_disk_masstransfer_CATEGORY_HOT", "RLOF_total_time_spent_disk_masstransfer_CATEGORY_PARTIALLY_THICK", "RLOF_total_time_spent_disk_masstransfer_CATEGORY_THICK", "RLOF_time_weighted_sum_synchronicity_factor", "RLOF_mass_weighted_sum_synchronicity_factor", "RLOF_episode_number", "RLOF_episode_initial_accretor_should_have_undergone_CHE", "RLOF_episode_initial_donor_should_have_undergone_CHE", "RLOF_episode_final_accretor_should_have_undergone_CHE", "RLOF_episode_final_donor_should_have_undergone_CHE"], "DCO_formation": ["uuid", "probability", "event_number", "event_type", "zams_mass_1", "zams_mass_2", "zams_orbital_period", "zams_separation", "zams_eccentricity", "time", "metallicity", "random_seed", "DCO_stellar_type_1", "DCO_stellar_type_2", "DCO_mass_1", "DCO_mass_2", "DCO_separation", "DCO_eccentricity", "DCO_period", "DCO_previous_separation", "DCO_previous_eccentricity", "DCO_previous_period", "DCO_formation_time_in_years", "DCO_inspiral_time_in_years", "DCO_merger_time_in_years", "DCO_total_rlof_episodes", "DCO_stable_rlof_episodes", "DCO_unstable_rlof_episodes"]}, "email_notifications_enabled": false, "email_notifications_APP_password": "", "email_notifications_recipients": [], "email_notifications_corresponding_email": "", "email_notification_extra_info_function_hook": null, "_time_elapsed": 7.152557373046875e-07, "code_string": "import math\nimport numpy as np\nfrom collections import OrderedDict\nfrom binarycpython.utils.useful_funcs import *\n\n\ndef grid_code(self, print_results=True):\n    # Grid code generated on 2023-05-19T16:07:21.017142\n    # This function generates the systems that will be evolved with binary_c\n\n    # Set initial values\n    _total_starcount = 0\n    starcounts = [0 for i in range(5)]\n    parameter_dict = {}\n    phasevol = 1\n    M_1 = None\n    M_2 = None\n    M_3 = None\n    M_4 = None\n    orbital_period = None\n    orbital_period_triple = None\n    orbital_period_quadruple = None\n    eccentricity = None\n    eccentricity_triple = None\n    eccentricity_quadruple = None\n    \n    # set probability objects\n    probabilities = {}\n    probabilities_list = [0 for i in range(5)]\n    probabilities_sum = [0 for i in range(5)]\n    probabilities[\"multiplicity\"] = 0\n    probabilities[\"lnM_1\"] = 0\n    probabilities[\"log10per\"] = 0\n    probabilities[\"q\"] = 0\n    \n    # for loop for variable multiplicity gridtype discrete\n    sampled_values_multiplicity = self.const_int(1, 2, 2)\n    for multiplicity_sample_number in range(0,len(sampled_values_multiplicity)+0):\n        multiplicity_this_index = multiplicity_sample_number         \n        multiplicity_prev_index = None if multiplicity_this_index == 0 else (multiplicity_this_index - 1)         \n        \n        multiplicity_next_index = None if multiplicity_this_index >= (len(sampled_values_multiplicity)+0 - 1) else (multiplicity_this_index + 1)        \n        dphasevol_multiplicity = 1.0 # 666\n        if dphasevol_multiplicity <= 0:\n            print(\"Grid generator: dphasevol_multiplicity <= 0! (this=\",multiplicity_this_index,\"=\",sampled_values_multiplicity[multiplicity_this_index],\", next=\",multiplicity_next_index,\"=\",sampled_values_multiplicity[multiplicity_next_index],\") Skipping current sample.\")\n            continue\n        multiplicity = sampled_values_multiplicity[multiplicity_this_index]\n        # Condition for multiplicity\n        if not ([0, 1, 0, 0][int(multiplicity)-1] > 0):\n            continue\n        \n        \n        self.population_options[\"multiplicity\"] = multiplicity; self.bse_options[\"multiplicity\"] = multiplicity; options={'q_high_extrapolation_method': 'flat', 'Mmin': 0.08, 'samplerfuncs': {'M': [None, None, None, None], 'logP': [None, None, None], 'ecc': [None, None, None]}, 'IMF_distribution': 'kroupa2001', 'JSON': None, 'q_low_extrapolation_method': 'flat', 'multiplicity_model': 'Poisson', 'normalize_multiplicities': 'merge', 'setup grid': True, 'clean load flag': False, 'apply settings': True, 'clean cache': False, 'load data': True, 'clean all': False, 'ranges': {'q': [None, None], 'ecc': [0.0, 0.99], 'M': [0.084, 120], 'logP': [0.0, 8.0]}, 'resolutions': {'ecc': [0, 0, 0], 'M': [80, 80, 0, 0], 'logP': [80, 0, 0]}, 'multiplicity_modulator': [0, 1, 0, 0]}\n        phasevol *= dphasevol_multiplicity\n        \n        # Set probabilities\n        dprob_multiplicity = dphasevol_multiplicity * (1)\n        probabilities_sum[0] += dprob_multiplicity\n        probabilities_list[0] = dprob_multiplicity\n        \n        # Increment starcount for multiplicity\n        starcounts[0] += 1\n        parameter_dict[\"multiplicity\"] = multiplicity\n        \n        # for loop for variable lnM_1 gridtype centred\n        sampled_values_lnM_1 = self.const_linear(np.log(0.084), np.log(120), 80)\n        for lnM_1_sample_number in range(0,len(sampled_values_lnM_1)+-1):\n            if lnM_1_sample_number == 0:\n                lnM_1_this_index = 0;\n            else:\n                lnM_1_this_index = lnM_1_sample_number             \n            lnM_1_prev_index = (lnM_1_this_index - 1) if lnM_1_this_index > 0 else None             \n            lnM_1_next_index = lnM_1_this_index + 1            \n            dphasevol_lnM_1 = (sampled_values_lnM_1[lnM_1_next_index] - sampled_values_lnM_1[lnM_1_this_index])\n            if dphasevol_lnM_1 <= 0:\n                print(\"Grid generator: dphasevol_lnM_1 <= 0! (this=\",lnM_1_this_index,\"=\",sampled_values_lnM_1[lnM_1_this_index],\", next=\",lnM_1_next_index,\"=\",sampled_values_lnM_1[lnM_1_next_index],\") Skipping current sample.\")\n                continue\n            lnM_1 = 0.5 * (sampled_values_lnM_1[lnM_1_next_index] + sampled_values_lnM_1[lnM_1_this_index])\n            \n            M_1 = np.exp(lnM_1); options[\"M_1\"]=M_1\n            phasevol *= dphasevol_lnM_1\n            \n            # Set probabilities\n            dprob_lnM_1 = dphasevol_lnM_1 * (self.Moe_di_Stefano_2017_pdf({'q_high_extrapolation_method': 'flat', 'Mmin': 0.08, 'samplerfuncs': {'M': [None, None, None, None], 'logP': [None, None, None], 'ecc': [None, None, None]}, 'IMF_distribution': 'kroupa2001', 'JSON': None, 'q_low_extrapolation_method': 'flat', 'multiplicity_model': 'Poisson', 'normalize_multiplicities': 'merge', 'setup grid': True, 'clean load flag': False, 'apply settings': True, 'clean cache': False, 'load data': True, 'clean all': False, 'ranges': {'q': [None, None], 'ecc': [0.0, 0.99], 'M': [0.084, 120], 'logP': [0.0, 8.0]}, 'resolutions': {'ecc': [0, 0, 0], 'M': [80, 80, 0, 0], 'logP': [80, 0, 0]}, 'multiplicity_modulator': [0, 1, 0, 0], 'multiplicity': multiplicity, 'M_1': M_1}, verbosity=self.population_options['verbosity'])['total_probdens'] if multiplicity == 1 else 1)\n            probabilities_sum[1] += dprob_lnM_1\n            probabilities_list[1] = probabilities_list[0] * dprob_lnM_1\n            \n            # Increment starcount for lnM_1\n            starcounts[1] += 1\n            parameter_dict[\"M_1\"] = M_1\n            \n            # for loop for variable log10per gridtype centred\n            sampled_values_log10per = self.const_linear(0.0, 8.0, 80)\n            for log10per_sample_number in range(0,len(sampled_values_log10per)+-1):\n                if log10per_sample_number == 0:\n                    log10per_this_index = 0;\n                else:\n                    log10per_this_index = log10per_sample_number                 \n                log10per_prev_index = (log10per_this_index - 1) if log10per_this_index > 0 else None                 \n                log10per_next_index = log10per_this_index + 1                \n                dphasevol_log10per = (sampled_values_log10per[log10per_next_index] - sampled_values_log10per[log10per_this_index])\n                if dphasevol_log10per <= 0:\n                    print(\"Grid generator: dphasevol_log10per <= 0! (this=\",log10per_this_index,\"=\",sampled_values_log10per[log10per_this_index],\", next=\",log10per_next_index,\"=\",sampled_values_log10per[log10per_next_index],\") Skipping current sample.\")\n                    continue\n                log10per = 0.5 * (sampled_values_log10per[log10per_next_index] + sampled_values_log10per[log10per_this_index])\n                # Condition for log10per\n                if not (self.population_options[\"multiplicity\"] >= 2):\n                    continue\n                \n                \n                orbital_period = 10.0**log10per\n                qmin=0.08/M_1\n                qmax=maximum_mass_ratio_for_RLOF(M_1, orbital_period)\n                \n                phasevol *= dphasevol_log10per\n                \n                # Set probabilities\n                dprob_log10per = dphasevol_log10per * (1.0)\n                probabilities_sum[2] += dprob_log10per\n                probabilities_list[2] = probabilities_list[1] * dprob_log10per\n                \n                # Increment starcount for log10per\n                starcounts[2] += 1\n                parameter_dict[\"orbital_period\"] = orbital_period\n                \n                # for loop for variable q gridtype centred\n                sampled_values_q = self.const_linear(0.08/M_1, qmax, 80)\n                for q_sample_number in range(0,len(sampled_values_q)+-1):\n                    if q_sample_number == 0:\n                        q_this_index = 0;\n                    else:\n                        q_this_index = q_sample_number                     \n                    q_prev_index = (q_this_index - 1) if q_this_index > 0 else None                     \n                    q_next_index = q_this_index + 1                    \n                    dphasevol_q = (sampled_values_q[q_next_index] - sampled_values_q[q_this_index])\n                    if dphasevol_q <= 0:\n                        print(\"Grid generator: dphasevol_q <= 0! (this=\",q_this_index,\"=\",sampled_values_q[q_this_index],\", next=\",q_next_index,\"=\",sampled_values_q[q_next_index],\") Skipping current sample.\")\n                        continue\n                    q = 0.5 * (sampled_values_q[q_next_index] + sampled_values_q[q_this_index])\n                    \n                    \n                    M_2 = q * M_1\n                    sep = calc_sep_from_period(M_1, M_2, orbital_period)\n                        \n                    phasevol *= dphasevol_q\n                    \n                    # Set probabilities\n                    dprob_q = dphasevol_q * (self.Moe_di_Stefano_2017_pdf({'q_high_extrapolation_method': 'flat', 'Mmin': 0.08, 'samplerfuncs': {'M': [None, None, None, None], 'logP': [None, None, None], 'ecc': [None, None, None]}, 'IMF_distribution': 'kroupa2001', 'JSON': None, 'q_low_extrapolation_method': 'flat', 'multiplicity_model': 'Poisson', 'normalize_multiplicities': 'merge', 'setup grid': True, 'clean load flag': False, 'apply settings': True, 'clean cache': False, 'load data': True, 'clean all': False, 'ranges': {'q': [None, None], 'ecc': [0.0, 0.99], 'M': [0.084, 120], 'logP': [0.0, 8.0]}, 'resolutions': {'ecc': [0, 0, 0], 'M': [80, 80, 0, 0], 'logP': [80, 0, 0]}, 'multiplicity_modulator': [0, 1, 0, 0], \"multiplicity\": multiplicity, \"M_1\": M_1, \"M_2\": M_2, \"M_3\": M_3, \"M_4\": M_4, \"P\": orbital_period, \"P2\": orbital_period_triple, \"P3\": orbital_period_quadruple, \"ecc\": eccentricity, \"ecc2\": eccentricity_triple, \"ecc3\": eccentricity_quadruple}, verbosity=self.population_options['verbosity'])['total_probdens'])\n                    probabilities_sum[3] += dprob_q\n                    probabilities_list[3] = probabilities_list[2] * dprob_q\n                    \n                    # Increment starcount for q\n                    starcounts[3] += 1\n                    parameter_dict[\"M_2\"] = M_2\n                    \n                    ########################################\n                    # grid sampling system call section (q)\n\n                    # Weigh the probability by a custom weighting factor\n                    probability = self.population_options[\"weight\"] * probabilities_list[3]\n                    \n                    # Factor the multiplicity fraction into the probability\n                    probability *= self._calculate_multiplicity_fraction(parameter_dict)\n                    \n                    # Divide the probability by the number of repeats\n                    probability /= self.population_options[\"repeat\"]\n                    \n                    # Loop over the repeats\n                    for _ in range(self.population_options[\"repeat\"]):\n                        _total_starcount += 1\n                        parameter_dict[\"probability\"] = probability\n                        parameter_dict[\"phasevol\"] = phasevol\n                        self._increment_probtot(probability)\n                        yield(parameter_dict)\n                    ########################################\n                    \n                    ########################################\n                    # Code below is for finalising the handling of this iteration of the parameter q\n\n                    phasevol /= dphasevol_q\n\n                ########################################\n                # Code below is for finalising the handling of this iteration of the parameter log10per\n\n                phasevol /= dphasevol_log10per\n\n            ########################################\n            # Code below is for finalising the handling of this iteration of the parameter lnM_1\n\n            ########################################\n            # Branch code\n            if multiplicity == 1:\n                ########################################\n                # grid sampling system call section (lnM_1)\n\n                # Weigh the probability by a custom weighting factor\n                probability = self.population_options[\"weight\"] * probabilities_list[1]\n                \n                # Factor the multiplicity fraction into the probability\n                probability *= self._calculate_multiplicity_fraction(parameter_dict)\n                \n                # Divide the probability by the number of repeats\n                probability /= self.population_options[\"repeat\"]\n                \n                # Loop over the repeats\n                for _ in range(self.population_options[\"repeat\"]):\n                    _total_starcount += 1\n                    parameter_dict[\"probability\"] = probability\n                    parameter_dict[\"phasevol\"] = phasevol\n                    self._increment_probtot(probability)\n                    yield(parameter_dict)\n                ########################################\n                \n            ########################################\n            \n            phasevol /= dphasevol_lnM_1\n\n        ########################################\n        # Code below is for finalising the handling of this iteration of the parameter multiplicity\n\n        phasevol /= dphasevol_multiplicity\n\n    \n    ########################################\n    if print_results:\n        print('Grid has handled {starcount} stars with a total probability of {probtot:g}'.format(starcount=_total_starcount,probtot=self.population_options['_probtot']))\n", "multiplicity": 2, "_job_crashed": false}, "custom_options": {"david_rlof_episode_logging": 0, "binary_c_python_scripts_git_info": {"datetime_string": "2023-05-19#15:48:48.384598", "repo_name": "binary_c_python_scripts", "branch_name": "versions/2.2.4-server", "commit_sha": "a88756d075a1b4aa1b1aecc4f7e350b63e9f0cc4"}, "data_dir": "/vol/ph/astro_data/dhendriks/binary_c_results/RLOF/EVENTS_V2.2.4_HIGH_RES_EXPLORATION_BALLISTIC_RLOF_2021_MOE_DISTEFANO/population_results/Z0.02"}}, "binary_c_defaults": {"defaults_set": "2022a", "skip_bad_args": "0", "metallicity": "0.02", "effective_metallicity": "-1", "M_1": "0", "M_2": "0", "M_3": "0", "M_4": "0", "vrot1": "0", "vrot2": "0", "vrot3": "0", "vrot4": "0", "fKerr1": "0", "fKerr2": "0", "fKerr3": "0", "fKerr4": "0", "vrot_multiplier1": "1", "vrot_multiplier2": "1", "vrot_multiplier3": "1", "vrot_multiplier4": "1", "Prot1": "0", "Prot2": "0", "Prot3": "0", "Prot4": "0", "inclination1": "0", "inclination2": "0", "inclination3": "0", "inclination4": "0", "B_1": "0", "B_2": "0", "B_3": "0", "B_4": "0", "B_inclination1": "0", "B_inclination2": "0", "B_inclination3": "0", "B_inclination4": "0", "separation": "0", "separation_triple": "0", "separation_quadruple": "0", "orbital_period": "0", "orbital_period_triple": "0", "orbital_period_quadruple": "0", "eccentricity": "0", "eccentricity_triple": "0", "eccentricity_quadruple": "0", "incliniation": "0", "incliniation_triple": "0", "incliniation_quadruple": "0", "orbital_phase": "0", "orbital_phase_triple": "0", "orbital_phase_quadruple": "0", "argument_of_periastron": "0", "argument_of_periastron_triple": "0", "argument_of_periastron_quadruple": "0", "stellar_type_1": "0", "stellar_type_2": "0", "stellar_type_3": "0", "stellar_type_4": "0", "max_stellar_type_1": "16", "max_stellar_type_2": "16", "max_stellar_type_3": "16", "max_stellar_type_4": "16", "probability": "1", "phasevol": "NULL", "stellar_structure_algorithm": "0", "solver": "0", "max_evolution_time": "15000", "max_model_number": "0", "monte_carlo_kicks": "True", "disable_debug": "False", "debug_filter_pointers": "False", "timestep_logging": "False", "flush_log": "False", "derivative_logging": "False", "progress_bar": "False", "log_all_reject_timestep_failures": "False", "cannot_shorten_timestep_policy": "0", "rejects_in_log": "False", "vandenHeuvel_logging": "False", "disc_timestep_factor": "0.01", "white_dwarf_cooling_model": "0", "white_dwarf_radius_model": "0", "cbdisc_mass_loss_inner_viscous_accretion_method": "0", "cbdisc_inner_edge_stripping": "True", "cbdisc_end_evolution_after_disc": "False", "cbdisc_no_wind_if_cbdisc": "False", "cbdisc_outer_edge_stripping": "True", "disc_n_monte_carlo_guesses": "0", "disc_log": "0", "disc_log2d": "0", "disc_log_dt": "0", "disc_log_directory": "/tmp/", "post_ce_adaptive_menv": "False", "post_ce_objects_have_envelopes": "False", "PN_comenv_transition_time": "100", "minimum_time_between_PNe": "0.1", "PN_Hall_fading_time_algorithm": "0", "PPN_envelope_mass": "0.01", "cbdisc_eccentricity_pumping_method": "1", "cbdisc_viscous_photoevaporative_coupling": "1", "cbdisc_inner_edge_stripping_timescale": "1", "cbdisc_outer_edge_stripping_timescale": "1", "cbdisc_viscous_L2_coupling": "1", "gravitational_radiation_model": "0", "nova_irradiation_multiplier": "0", "gravitational_radiation_modulator_J": "1", "gravitational_radiation_modulator_e": "1", "nova_faml_multiplier": "0", "RLOF_angular_momentum_transfer_model": "0", "post_SN_orbit_method": "1", "evolution_splitting": "False", "disable_events": "False", "evolution_splitting_sn_eccentricity_threshold": "0.01", "evolution_splitting_sn_n": "10", "evolution_splitting_maxdepth": "2", "random_seed": "0", "random_systems_seed": "0", "random_skip": "0", "idum": "0", "repeat": "1", "pause_after_repeat": "False", "random_systems": "0", "equation_of_state_algorithm": "NULL", "opacity_algorithm": "NULL", "wind_mass_loss": "3", "multiplicity": "0", "gbwind": "0", "postagbwind": "0", "Teff_postAGB_min": "6000", "Teff_postAGB_max": "120000", "mattsson_Orich_tpagbwind": "NULL", "magnetic_braking_factor": "1", "magnetic_braking_gamma": "3", "magnetic_braking_algorithm": "0", "helium_flash_mass_loss": "0", "gb_reimers_eta": "0.4", "gbwindfac": "1", "tpagbwindfac": "1", "eagbwindfac": "1", "nieuwenhuijzen_windfac": "1", "tpagbwind": "0", "eagbwind": "0", "wind_gas_to_dust_ratio": "200", "vwind_multiplier": "1", "vwind_beta": "0.125", "superwind_mira_switchon": "500", "vw93_mira_shift": "0", "vw93_multiplier": "1", "tpagb_reimers_eta": "1", "Tout_Pringle_1992_multiplier": "0", "artificial_mass_accretion_rate%d": "", "artificial_mass_accretion_rate_by_stellar_type%d": "", "artificial_angular_momentum_accretion_rate%d": "", "artificial_orbital_angular_momentum_accretion_rate": "0", "artificial_accretion_start_time": "-1", "artificial_accretion_end_time": "-1", "wr_wind": "0", "wr_wind_fac": "1", "wrwindfac": "1", "accretion_limit_eddington_steady_multiplier": "1", "accretion_limit_eddington_LMMS_multiplier": "1", "accretion_limit_eddington_WD_to_remnant_multiplier": "-1", "accretion_limit_thermal_multiplier": "1", "accretion_limit_dynamical_multiplier": "1", "donor_limit_envelope_multiplier": "0", "donor_limit_thermal_multiplier": "1", "donor_limit_dynamical_multiplier": "1", "Bondi_Hoyle_accretion_factor": "1.5", "BH_prescription": "0", "sn_kick_distribution_II": "1", "sn_kick_distribution_ECAP": "0", "sn_kick_distribution_NS_NS": "0", "sn_kick_distribution_IBC": "1", "sn_kick_distribution_GRB_COLLAPSAR": "1", "sn_kick_distribution_TZ": "0", "sn_kick_distribution_AIC_BH": "0", "sn_kick_distribution_BH_BH": "0", "sn_kick_distribution_BH_NS": "0", "sn_kick_distribution_IA_Hybrid_HeCOWD": "0", "sn_kick_distribution_IA_Hybrid_HeCOWD_subluminous": "0", "sn_kick_dispersion_II": "190", "sn_kick_dispersion_ECAP": "0", "sn_kick_dispersion_NS_NS": "0", "sn_kick_dispersion_IBC": "190", "sn_kick_dispersion_GRB_COLLAPSAR": "190", "sn_kick_dispersion_TZ": "0", "sn_kick_dispersion_AIC_BH": "0", "sn_kick_dispersion_BH_BH": "0", "sn_kick_dispersion_BH_NS": "0", "sn_kick_dispersion_IA_Hybrid_HeCOWD": "0", "sn_kick_dispersion_IA_Hybrid_HeCOWD_subluminous": "0", "sn_kick_companion_IA_He": "0", "sn_kick_companion_IA_ELD": "0", "sn_kick_companion_IA_CHAND": "0", "sn_kick_companion_AIC": "0", "sn_kick_companion_ECAP": "0", "sn_kick_companion_IA_He_Coal": "0", "sn_kick_companion_IA_CHAND_Coal": "0", "sn_kick_companion_NS_NS": "0", "sn_kick_companion_GRB_COLLAPSAR": "0", "sn_kick_companion_HeStarIa": "0", "sn_kick_companion_IBC": "0", "sn_kick_companion_II": "0", "sn_kick_companion_IIa": "0", "sn_kick_companion_WDKICK": "0", "sn_kick_companion_TZ": "0", "sn_kick_companion_AIC_BH": "0", "sn_kick_companion_BH_BH": "0", "sn_kick_companion_BH_NS": "0", "sn_kick_companion_IA_Hybrid_HeCOWD": "0", "sn_kick_companion_IA_Hybrid_HeCOWD_subluminous": "0", "wd_sigma": "0", "wd_kick_direction": "0", "wd_kick_when": "0", "wd_kick_pulse_number": "0", "minimum_helium_ignition_core_mass": "0", "minimum_CO_core_mass_for_carbon_ignition": "1.08", "minimum_CO_core_mass_for_neon_ignition": "1.42", "minimum_mcbagb_for_nondegenerate_carbon_ignition": "2.25", "maximum_mcbagb_for_degenerate_carbon_ignition": "1.6", "max_neutron_star_mass": "2.2", "chandrasekhar_mass": "1.38", "delta_mcmin": "NULL", "lambda_min": "NULL", "lambda_multiplier": "NULL", "minimum_envelope_mass_for_third_dredgeup": "NULL", "cf_amanda_log": "NULL", "float_overflow_checks": "0", "save_pre_events_stardata": "False", "disable_end_logging": "False", "mass_of_pmz": "NULL", "c13_eff": "NULL", "mc13_pocket_multiplier": "NULL", "tides_convective_damping": "0", "E2_prescription": "0", "dtfac": "1", "hbbtfac": "NULL", "tidal_strength_factor": "1", "tides_variable_filename": "empty_string", "hachisu_qcrit": "1.15", "hachisu_disk_wind": "False", "mass_accretion_for_eld": "0.15", "WDWD_merger_algorithm": "0", "eta_violent_WDWD_merger": "0.75", "COWD_COWD_explode_above_mass": "0", "HeWD_COWD_explode_above_mass": "0", "COWD_to_ONeWD_accretion_rate": "2.05e-06", "type_Ia_MCh_supernova_algorithm": "NULL", "core_collapse_supernova_algorithm": "NULL", "electron_capture_supernova_algorithm": "NULL", "core_collapse_rprocess_algorithm": "NULL", "core_collapse_rprocess_mass": "NULL", "Seitenzahl2013_model": "NULL", "type_Ia_sub_MCh_supernova_algorithm": "NULL", "max_HeWD_mass": "0.7", "merger_mass_loss_fraction": "0.1", "merger_mass_loss_fraction_nondegenerate": "NULL", "merger_mass_loss_fraction_degenerate": "NULL", "merger_mass_loss_fraction_by_stellar_type_%d": "", "transient_method": "0", "merger_angular_momentum_factor": "1", "wind_angular_momentum_loss": "0", "wind_djorb_fac": "1", "lw": "1", "VW93_EAGB_wind_speed": "False", "VW93_TPAGB_wind_speed": "False", "ensemble": "False", "ensemble_filters_off": "False", "ensemble_filter_%d": "", "ensemble_legacy_ensemble": "False", "legacy_yields": "NULL", "ensemble_defer": "False", "ensemble_dt": "1", "ensemble_logdt": "0.1", "ensemble_startlogtime": "0.1", "ensemble_logtimes": "False", "postagb_legacy_logging": "False", "disc_legacy_logging": "False", "wind_multiplier_%d": "", "wind_type_multiplier_%d": "", "reverse_time": "NULL", "start_time": "0", "EMP_logg_maximum": "NULL", "EMP_minimum_age": "NULL", "EMP_feh_maximum": "NULL", "CEMP_cfe_minimum": "NULL", "NEMP_cfe_minimum": "NULL", "thick_disc_start_age": "NULL", "thick_disc_end_age": "NULL", "thick_disc_logg_min": "NULL", "thick_disc_logg_max": "NULL", "escape_velocity": "NULL", "escape_fraction": "NULL", "pre_main_sequence": "False", "pre_main_sequence_fit_lobes": "False", "use_periastron_Roche_radius": "False", "qcrit_nuclear_burning": "NULL", "qcrit_WD": "NULL", "qcrit_all": "NULL", "qcrit_LMMS": "0.6944", "qcrit_MS": "1.6", "qcrit_HG": "4", "qcrit_GB": "-1", "qcrit_CHeB": "3", "qcrit_EAGB": "-1", "qcrit_TPAGB": "-1", "qcrit_HeMS": "3", "qcrit_HeHG": "4", "qcrit_HeGB": "0.78125", "qcrit_HeWD": "3", "qcrit_COWD": "3", "qcrit_ONeWD": "3", "qcrit_NS": "3", "qcrit_BH": "3", "qcrit_degenerate_LMMS": "1", "qcrit_degenerate_MS": "1", "qcrit_degenerate_HG": "4.7619", "qcrit_degenerate_GB": "1.15", "qcrit_degenerate_CHeB": "3", "qcrit_degenerate_EAGB": "1.15", "qcrit_degenerate_TPAGB": "1.15", "qcrit_degenerate_HeMS": "3", "qcrit_degenerate_HeHG": "4.7619", "qcrit_degenerate_HeGB": "1.15", "qcrit_degenerate_HeWD": "0.625", "qcrit_degenerate_COWD": "0.625", "qcrit_degenerate_ONeWD": "0.625", "qcrit_degenerate_NS": "0.625", "qcrit_degenerate_BH": "0.625", "mass_for_Hestar_Ia_upper": "0", "mass_for_Hestar_Ia_lower": "0", "alphaCB": "NULL", "minimum_donor_menv_for_comenv": "0", "comenv_prescription": "0", "comenv_prescription%d": "", "comenv_ejection_spin_method": "0", "comenv_merger_spin_method": "0", "comenv_ms_accretion_mass": "NULL", "comenv_ms_accretion_fraction": "NULL", "comenv_ns_accretion_mass": "NULL", "comenv_ns_accretion_fraction": "NULL", "alpha_ce": "1", "alpha_ce%d": "", "lambda_ce": "0.5", "lambda_ce%d": "", "comenv_splitmass": "NULL", "nelemans_recalc_eccentricity": "False", "comenv_post_eccentricity": "1e-05", "dedmRLOF": "0", "nelemans_gamma": "1.75", "nelemans_minq": "0.2", "nelemans_max_frac_j_change": "1", "nelemans_n_comenvs": "1", "lambda_ionisation": "0.5", "lambda_ionisation%d": "", "lambda_enthalpy": "0", "lambda_enthalpy%d": "", "cbdisc_albedo": "0", "cbdisc_gamma": "1.4", "cbdisc_alpha": "0.001", "cbdisc_kappa": "0.01", "cbdisc_minimum_evaporation_timescale": "1", "cbdisc_torquef": "0.001", "cbdisc_max_lifetime": "1e+06", "cbdisc_init_dM": "0.1", "cbdisc_init_dJdM": "0.5", "cbdisc_mass_loss_constant_rate": "0", "cbdisc_mass_loss_FUV_multiplier": "1", "cbdisc_mass_loss_Xray_multiplier": "1", "cbdisc_mass_loss_ISM_ram_pressure_multiplier": "1", "cbdisc_mass_loss_ISM_pressure": "3000", "cbdisc_mass_loss_inner_viscous_multiplier": "1", "cbdisc_mass_loss_inner_viscous_angular_momentum_multiplier": "1", "cbdisc_resonance_multiplier": "1", "cbdisc_resonance_damping": "True", "cbdisc_fail_ring_inside_separation": "False", "cbdisc_mass_loss_inner_L2_cross_multiplier": "1", "cbdisc_minimum_luminosity": "0", "cbdisc_minimum_mass": "1e-06", "cbdisc_minimum_fRing": "0.2", "comenv_disc_angmom_fraction": "0", "comenv_disc_mass_fraction": "0", "wind_disc_angmom_fraction": "0", "wind_disc_mass_fraction": "0", "WRLOF_method": "0", "minimum_timestep": "1e-06", "timestep_solver_factor": "1", "RLOF_mdot_factor": "1", "RLOF_f": "NULL", "unstable_RLOF_can_trigger_SNIa": "False", "triggered_SNIa_algorithm": "NULL", "minimum_separation_for_instant_RLOF": "False", "minimum_orbital_period_for_instant_RLOF": "False", "maximum_mass_ratio_for_instant_RLOF": "False", "RLOF_method": "0", "small_envelope_method": "0", "RLOF_interpolation_method": "0", "timestep_modulator": "1", "timestep_multiplier%d": "", "maximum_timestep": "1e+20", "maximum_timestep_by_stellar_type_%d": "", "zoomfac_multiplier_decrease": "0.5", "zoomfac_multiplier_increase": "1.2", "maximum_timestep_factor": "0", "maximum_nuclear_burning_timestep": "1e+20", "nova_retention_method": "0", "nova_yield_CO_algorithm": "NULL", "nova_yield_ONe_algorithm": "NULL", "He_nova_ELDs": "False", "nova_retention_fraction_H": "0.001", "nova_retention_fraction_He": "0.001", "beta_reverse_nova": "0", "WD_accretion_rate_nalgorithms": "NULL", "WD_accretion_rate_novae_upper_limit_hydrogen_donor": "-1", "WD_accretion_rate_novae_upper_limit_helium_donor": "-1", "WD_accretion_rate_novae_upper_limit_other_donor": "-1", "WD_accretion_rate_new_giant_envelope_lower_limit_hydrogen_donor": "-1", "WD_accretion_rate_new_giant_envelope_lower_limit_helium_donor": "-1", "WD_accretion_rate_new_giant_envelope_lower_limit_other_donor": "-1", "CRAP_parameter": "0", "colour_log": "False", "log_legacy_stellar_types": "False", "log_filename": "/tmp/c_log.dat", "log_separator": "empty_string", "log_period_unit": "0", "clean_log": "False", "log_arrows": "False", "stopfile": "empty_string", "MINT_metallicity": "-1", "MINT_dir": "empty_string", "MINT_load_state_file": "empty_string", "MINT_save_state_file": "empty_string", "MINT_data_cleanup": "False", "MINT_MS_rejuvenation": "True", "MINT_remesh": "True", "MINT_filename_vb": "False", "MINT_use_ZAMS_profiles": "True", "MINT_fallback_to_test_data": "False", "MINT_use_fallback_comenv": "False", "MINT_disable_grid_load_warnings": "False", "MINT_disable_warnings": "False", "MINT_Kippenhahn": "0", "MINT_nshells": "200", "MINT_maximum_nshells": "1000", "MINT_minimum_nshells": "10", "MINT_Kippenhahn_stellar_type": "-1", "MINT_Kippenhahn_companion_stellar_type": "-1", "MINT_nuclear_burning": "False", "MINT_minimum_shell_mass": "1e-06", "MINT_maximum_shell_mass": "0.1", "stardata_dump_filename": "empty_string", "stardata_load_filename": "empty_string", "api_log_filename_prefix": "/dev/null", "hrdiag_output": "NULL", "internal_buffering": "2", "individual_novae": "False", "nova_timestep_accelerator_num": "100", "nova_timestep_accelerator_index": "0.5", "nova_timestep_accelerator_max": "-1", "eccentric_RLOF_model": "0", "force_circularization_on_RLOF": "True", "resolve_stellar_type_changes": "False", "nonconservative_angmom_gamma": "-1", "max_stellar_angmom_change": "0.05", "third_dup": "True", "third_dup_multiplier": "NULL", "NeNaMgAl": "NULL", 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{"KICK_BACKWARD": "3", "KICK_FORWARD": "2", "KICK_INWARD": "4", "KICK_OUTWARD": "5", "KICK_RANDOM": "0", "KICK_STRAIGHT_UP": "1"}, "wd_kick_when": {"WD_KICK_AT_EVERY_PULSE": "3", "WD_KICK_AT_GIVEN_PULSE": "2", "WD_KICK_END_AGB": "0", "WD_KICK_FIRST_RLOF": "1"}, "white_dwarf_cooling_model": {"WHITE_DWARF_COOLING_CARRASCO2014": "2", "WHITE_DWARF_COOLING_MESTEL": "0", "WHITE_DWARF_COOLING_MESTEL_MODIFIED": "1"}, "white_dwarf_radius_model": {"WHITE_DWARF_RADIUS_CARRASCO2014": "2", "WHITE_DWARF_RADIUS_MU": "1", "WHITE_DWARF_RADIUS_NAUENBERG1972": "0"}, "wind_angular_momentum_loss": {"WIND_ANGMOM_LOSS_BSE": "0", "WIND_ANGMOM_LOSS_LW": "1", "WIND_ANGMOM_LOSS_LW_HYBRID": "2", "WIND_ANGMOM_LOSS_SPHERICALLY_SYMMETRIC": "3"}, "wind_mass_loss": {"WIND_ALGORITHM_BINARY_C_2020": "3", "WIND_ALGORITHM_BINARY_C_2022": "5", "WIND_ALGORITHM_HENDRIKS_2022": "4", "WIND_ALGORITHM_HURLEY2002": "1", "WIND_ALGORITHM_NONE": "0", "WIND_ALGORITHM_SCHNEIDER2018": "2"}, "wr_wind": {"WR_WIND_BSE": "0", 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"362": "PERETS_HeWD_GT0p3_COWD_LT0p6", "401": "MERGER_LMMS_Hybrid_HeCOWD", "260": "MERGER_NS_MS", "537": "SN_IA_Hybrid_HeCOWD_DARK", "268": "MERGER_HeHG_HG", "373": "TEST_RATE", "432": "TZ_M1_22_23", "489": "SN_BH_BH", "453": "MDOT_SAGB", "409": "MERGER_HeHG_Hybrid_HeCOWD", "407": "MERGER_TPAGB_Hybrid_HeCOWD", "304": "MERGER_COWD_EAGB", "170": "COMENV_HeGB_DETACHED", "342": "MERGER_BH_HeWD", "329": "MERGER_ONeWD_HeHG", "7": "WNL_LUM", "242": "MERGER_HeGB_LMMS", "426": "TZ_M1_16_17", "247": "MERGER_BH_LMMS", "19": "MS_LUM", "208": "MAGNITUDE_GAIA_GRP", "68": "SPECTRAL_TYPE_A_GIANT", "474": "SN_SubChandIa_CO", "340": "MERGER_ONeWD_HeWD", "535": "SN_BH_BH_DARK", "33": "HeHG_LUM", "53": "XRAY_WDXB_LUM", "203": "MAGNITUDE_f555w", "228": "MERGER_INTO_COWD", "414": "MERGER_NS_Hybrid_HeCOWD", "436": "TZ_M1_26_27", "320": "MERGER_HeWD_HeMS", "272": "MERGER_ONeWD_HG", "533": "SN_TZ_DARK", "415": "MERGER_BH_Hybrid_HeCOWD", "490": "SN_BH_NS", "107": "SPECTRAL_TYPE_Ba_SUPERGIANT", "509": "SN_WDKICK_BRIGHT", "510": "SN_TZ_BRIGHT", "99": "SPECTRAL_TYPE_S_DWARF", "201": "MAGNITUDE_f435w", "519": "SN_ChandIa_DARK", "117": "NSBH_DD", "84": "SPECTRAL_TYPE_K_DWARF", "497": "SN_SubChandIa_CO_BRIGHT", "118": "BHBH_DD", "64": "SPECTRAL_TYPE_B_DWARF", "39": "COWD_LUM", "158": "MASS_IN_BINARY_STARS", "306": "MERGER_NS_EAGB", "235": "MERGER_HG_LMMS", "294": "MERGER_COWD_CHeB", "496": "SN_ChandIa_BRIGHT", "185": "Be_XRB", "291": "MERGER_HeHG_CHeB", "324": "MERGER_BH_HeMS", "422": "TZ_M1_12_13", "410": "MERGER_HeGB_Hybrid_HeCOWD", "3": "WO", "343": "MERGER_COWD_COWD", "162": "LUMINOSITY_OF_RUNAWAY_STARS", "502": "SN_CHAND_Coal_BRIGHT", "429": "TZ_M1_19_20", "289": "MERGER_TPAGB_CHeB", "355": "PERETS_HeWD_COWD_LT0p8", "354": "DAVIES_RSG_LUM", "368": "PERETS_HeWD_LT0p25_COWD_LT0p5", "23": "GB_LUM", "457": "MDOT_SNIa_CHAND", "514": "SN_IA_Hybrid_HeCOWD_BRIGHT", "76": "SPECTRAL_TYPE_G", "194": "MAGNITUDE_u", "420": "TZ_M1_10_11", "176": "COMENV_TPAGB_MERGER", "74": 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"177": "COMENV_HeHG_MERGER", "385": "SUPERNOVA_CORE_COLLAPSE_LUMINOSITY", "222": "MERGER_INTO_EAGB", "95": "SPECTRAL_TYPE_C_LUM", "142": "SPECTRAL_TYPE_EXTRINSIC_GIANT_C_LUM", "261": "MERGER_BH_MS", "29": "TPAGB_LUM", "157": "MASS_IN_SINGLE_STARS", "234": "MERGER_MS_LMMS", "438": "TZ_M1_28_29", "104": "SPECTRAL_TYPE_Tc_DWARF", "452": "MDOT_TZ", "427": "TZ_M1_17_18", "278": "MERGER_TPAGB_GB", "215": "NUMBER_OF_OBSERVABLE_SINGLE_STARS", "397": "NOVA_MOMENTUM", "390": "WIND_ISG_MOMENTUM", "102": "SPECTRAL_TYPE_Tc_GIANT", "163": "MASS_IN_RUNAWAY_STARS", "383": "NOVA_KINETIC_POWER", "138": "LBV_LUM", "403": "MERGER_HG_Hybrid_HeCOWD", "286": "MERGER_BH_GB", "58": "SPECTRAL_TYPE_O_GIANT", "336": "MERGER_NS_HeGB", "377": "WIND_BSG_KINETIC_POWER", "44": "BH", "40": "ONeWD", "18": "MS", "248": "MERGER_MS_MS", "411": "MERGER_HeWD_Hybrid_HeCOWD", "199": "MAGNITUDE_f300w", "363": "PERETS_HeWD_GT0p3_COWD_LT0p5", "398": "MERGER_HeWD_gt_COWD", "121": "SYMBIOTIC_CV", "116": "NSNS_DD", "148": 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"Floating"}, "68": {"number": 68, "name": "BINARY_C_UPDATE_MASSES_MALLOC_FAILED", "description": "Update"}, "72": {"number": 72, "name": "BINARY_C_NINTLIB_EXIT", "description": "Nintlib"}, "27": {"number": 27, "name": "BINARY_C_XHBB_OR_XENV_CALLOC_FAILED", "description": "Xhbb"}, "26": {"number": 26, "name": "BINARY_C_MIX_MERGED_STELLAR_TYPE_NOT_CAUGHT", "description": "Mix"}, "85": {"number": 85, "name": "BINARY_C_STACK_FAIL", "description": "Stack"}, "40": {"number": 40, "name": "BINARY_C_DETAILED_LOG_OPEN_FAILED", "description": "Detailed"}, "16": {"number": 16, "name": "BINARY_C_ADAPTIVE_GRID_NO_SAVE_FILE_BACKUP", "description": "Adaptive"}, "38": {"number": 38, "name": "BINARY_C_LOG_FP_NULL_IN_ITERATE", "description": "Log"}, "11": {"number": 11, "name": "BINARY_C_GIANT_AGE_STAR_TOO_BIG_FOR_GB", "description": "Giant"}}, "deflists": {"stellar_type": {"4": "CHeB", "8": "HeHG", "0": "LOW_MASS_MS", "1": "MS", "11": "COWD", "7": "HeMS", "12": "ONeWD", "9": "HeGB", "3": "GIANT_BRANCH", "10": "HeWD", "5": "EAGB", "15": "MASSLESS_REMNANT", "6": "TPAGB", "2": "HG", "14": "BH", "13": "NS"}, "RLOF_stability_case": {"-2": "INSTABILITY_BLOCKED", "2": "UNSTABLE_LOW_MASS_MS_COMENV", "6": "UNSTABLE_BH", "0": "STABLE", "7": "UNSTABLE_MS_MERGER", "8": "UNSTABLE_VERY_LARGE_DONOR", "4": "UNSTABLE_WD_COMENV", "3": "UNSTABLE_GIANT_COMENV", "-1": "IMPOSSIBLE", "5": "UNSTABLE_NS", "1": "UNSTABLE"}, "sn_type": {"25": "PISN", "16": "WDKICK", "24": "PPISN", "21": "IA_Hybrid_HeCOWD", "23": "IA_Violent", "8": "He_Coal", "12": "HeStarIa", "15": "IIa", "1": "HeIa", "7": "ECAP", "17": "TZ", "26": "PHDIS", "9": "CHAND_Coal", "13": "Ib/c", "22": "IA_Hybrid_HeCOWD_subluminous", "2": "ELDIa", "20": "BH_NS", "3": "ChandIa", "6": "AIC", "11": "GRB_Collapsar", "18": "AIC_BH", "0": "None", "5": "SubChandIa_He", "10": "GRB_NS_NS", "14": "II", "4": "SubChandIa_CO", "19": "BH_BH"}, "RLOF_type": {"3": "C", "0": "NO_RLOF", "1": "A", "2": "B", "4": "OTHER"}}, "miscellaneous": {"git_revision": "6893:20230519:bc133b7", "git_url": "git@gitlab-dhendriks:binary_c/binary_c.git", "version": "2.2.4", "git_branch": "david/versions/2.2.4", "build": "May 19 2023 15:41:48", "email": ["r.izzard@surrey.ac.uk", " rob.izzard@gmail.com"], "Stellar derivative 36": "CO core mass", "Timestep multiplier 19": "STELLAR_ANGMOM", "Stellar derivative 20": "J RLOF Gain", "ANSI colour 15 BRIGHT_CYAN : Default": "\u001b[1;36m[1;36m\u001b[0;0m.", "System derivative 6": "J RLOF Loss", "MEGA_ELECTRON_VOLT_SI": "1.602176479703168350131535485094e-13", "System derivative 27": "Jorbit CS disc tides loss", "Timestep multiplier 40": "NOVAE", "Stellar derivative 39": "Fe core mass", "M_VENUS_SI": "4.869999999999999601541120000000e+24", "Timestep multiplier 59": "TIME_REMAINING", "Timestep multiplier 42": "SN", "ASTRONOMICAL_UNIT_SI": "1.495978707000000000000000000000e+11", "BINARY_C_TASK_NUMBER": "5", "A_JUPITER_SI": "7.786000000000000000000000000000e+10", "A_VENUS_SI": "1.082000000000000000000000000000e+10", "System derivative 13": "J artificial", "Timestep multiplier 48": "BURN_IN", "M_NEPTUNE_SI": "1.020000000000000079524003840000e+26", "Timestep multiplier 8": "EAGB", "Stellar derivative 55": "M CSdisc Transfer", "System derivative 9": "J tides", "Timestep multiplier 46": "NUCSYN_ANGELOU_LITHIUM", "M_JUPITER_SI": "1.898000000000000224781139968000e+27", "M_PLUTO_SI": "1.270000000000000104857600000000e+22", "Stellar derivative 17": "M Irradiative Loss", "Timestep multiplier 5": "HG", "Timestep multiplier 32": "FABIAN_IMF_LOG", "Timestep multiplier 49": "RADIUS_CHANGES", "M_EARTH_SI": "5.972200000000000224395264000000e+24", "TIDES": "deprecated! (always on)", "Stellar derivative 57": "M CSdisc Loss via L2", "Timestep multiplier 34": "HRD2", "Stellar derivative 8": "M RLOF Gain", "Stellar derivative 11": "M RLOF Gain through self accretion", "GAS_CONSTANT_SI": "8.314454122092682197830981749576e+00", "System derivative 1": "a", "Timestep multiplier 45": "TIDES", "System derivative 24": "Jorbit stream torque gain", "RYDBERG_ENERGY_SI": "2.179867831298505940947628311619e-18", "Stellar derivative 47": "He core mass (no 3DUP)", "ANSI colour 9 BOLD : Default": "\u001b[0;1m[0;1m\u001b[0;0m.", "Timestep multiplier 58": "FIXED_TIMESTEP", "Timestep multiplier 43": "MASS_GAIN", "ENSEMBLE_NUMBER": "540", "Byte order": "little endian", "Stellar derivative 6": "Stellar temperature", "System derivative 19": "Mdot Circumbinary Disc", "ALIGNSIZE": "not defined", "Stellar derivative 32": "eccentricity", "Timestep multiplier 57": "RLOF", "System derivative 26": "Jorbit CS disc tides gain", "Stellar derivative 54": "log(Central degeneracy)", "Stellar derivative 16": "M Non-conservative Loss", "M_SUN_SI": "1.989100000000000169284324032512e+30", "ANSI colour 7 CYAN : Default": "\u001b[0;36m[0;36m\u001b[0;0m.", "Timestep multiplier 11": "TPAGB", "System derivative 18": "e RLOF", "M_MARS_SI": "6.419999999999999119196160000000e+23", "ANSI colour 3 YELLOW : Default": "\u001b[0;33m[0;33m\u001b[0;0m.", "Stellar derivative 24": "J Magnetic Braking", "Stellar derivative 3": "Radius", "Stellar derivative 45": "Central carbon", "Stellar derivative 25": "J Decretion Disc", "Stellar derivative 14": "M Decretion Disc Loss", "System derivative 4": "J Wind Loss", "ANSI colour 4 ORANGE : Default": "\u001b[0;33m[0;33m\u001b[0;0m.", "System derivative 0": "J (total)", "ANSI colour 12 BRIGHT_YELLOW : Default": "\u001b[1;33m[1;33m\u001b[0;0m.", "Timestep multiplier 20": "STELLAR_MASS_LOSS", "M_PROTON_SI": "1.672620999999999936790515200999e-27", "Timestep multiplier 62": "NUMBER", "System derivative 22": "J self-accretion RLOF gain", "System derivative 7": "J RLOF Gain", "BOLOMETRIC_L0_SI": "3.012799999999999785385852928000e+28", "ANSI colour 18 UNDERLINE : Default": "\u001b[0;4m[0;4m\u001b[0;0m.", "Timestep multiplier 17": "HeHG_GB", "System derivative 16": "e Winds", "Stellar derivative 29": "J artificial", "Timestep multiplier 30": "CEMP_NEARLY", "Timestep multiplier 39": "MAXIMUM_TIMESTEP_BY_STELLAR_TYPE", "Timestep multiplier 33": "HRD1", "System derivative 31": "e Circumstellar Disc", "Timestep multiplier 23": "RESOLVE_POSTAGB", "EVOLUTION_SPLITTING": "on : EVOLUTION_SPLITTING_HARD_MAX_DEPTH=10 EVOLUTION_SPLITTING_MAX_SPLITDEPTH_DEFAULT=2 EVOLUTION_SPLITTING_SUPERNOVA_N=10", "M_SATURN_SI": "5.680000000000000119453777920000e+26", "Timestep multiplier 41": "ARTIFICIAL_ACCRETION", "ANSI colour 6 MAGENTA : Default": "\u001b[0;35m[0;35m\u001b[0;0m.", "Stellar derivative 46": "Central oxygen", "Stellar derivative 50": "nova H layer mass", "ANSI colour 0 BLACK : Default": "\u001b[0;30m[0;30m\u001b[0;0m.", "ANSI colour 16 BRIGHT_WHITE : Default": "\u001b[1;37m[1;37m\u001b[0;0m.", "A_EARTH_SI": "1.495978707000000000000000000000e+10", "System derivative 29": "J CSdisc isotropic mass loss", "Timestep multiplier 53": "TIDES2", "System derivative 20": "Test", "A_SATURN_SI": "1.433500000000000000000000000000e+11", "Timestep multiplier 0": "NONE", "Timestep multiplier 61": "THERMAL", "Stellar derivative 34": "He core mass", "Timestep multiplier 31": "CEMP_FLOOR", "Stellar derivative 9": "M Nova", "Stellar derivative 51": "nova He layer mass", "A_MARS_SI": "2.279000000000000000000000000000e+10", "Stellar derivative 53": "Number of novae", "Stellar derivative 27": "J Nova", "ANSI colour 11 BRIGHT_GREEN : Default": "\u001b[1;32m[1;32m\u001b[0;0m.", "Stellar derivative 59": "M CSdisc accretor Gain", "Stellar derivative 62": "J stream interaction", "TRUE tests - should all give No : \"T\" = No, \"t\" = No, \"TRUE\" = No, \"True\" = No, \"true\" = No, \"truE\" = No, \"on\" = No, \"On\" = No, \"ON\" = No, \"1\" = No, macroxyz MACRO : TIMER": "on", "System derivative 11": "J nova", "Timestep multiplier 29": "CEMP_EMP", "Timestep multiplier 13": "TPAGB_NUCSYN_SPEEDUP", "Stellar derivative 21": "J Wind Loss", "Timestep multiplier 44": "MASS_LOSS", "Timestep multiplier 3": "PREROCHE_MS", "ANSI colour 13 BRIGHT_BLUE : Default": "\u001b[1;34m[1;34m\u001b[0;0m.", "SIGMA_THOMPSON_SI": "6.652457186874891590722195299488e-29", "Timestep multiplier 7": "CHeB", "Stellar derivative 5": "Core Mass", "System derivative 25": "Jorbit stream torque loss", "Timestep multiplier 9": "EAGB_AXEL", "ANSI colour 8 WHITE : Default": "\u001b[0;37m[0;37m\u001b[0;0m.", "Stellar derivative 22": "J Wind Gain", "System derivative 10": "J nonconservative", "ANSI colour 2 GREEN : Default": "\u001b[0;32m[0;32m\u001b[0;0m.", "Timestep multiplier 47": "CARBON_BURNING", "Stellar derivative 10": "M RLOF Transfer", "M_MERCURY_SI": "3.300000000000000293601280000000e+23", "ELECTRON_CHARGE_SI": "1.602176479703168341626628850680e-19", "A_URANUS_SI": "2.872500000000000000000000000000e+11", "ADAPTIVE_RLOF ADAPTIVE_RLOF_IMIN=4 ADAPTIVE_RLOF_IMAX=10000 ADAPTIVE_RLOF_ALPHA=0.25 ADAPTIVE_RLOF_MINIMUM_RADIUS_ERROR=1e-06 ADAPTIVE_RLOF_MAX_ENV_FRAC=0.5 [ADAPTIVE_RLOF_DM_MAX=0.1 for M=10 and 0.2 for M=20] macroxyz MACRO : ADAPTIVE_RLOF_CONVECTIVE_CHECK": "off", "System derivative 17": "e Circumbinary Disc", "M_URANUS_SI": "8.680000000000000090596966400000e+25", "Stellar derivative 40": "Neutron core mass", "Timestep multiplier 55": "MASS_LOSS2", "Stellar derivative 63": "J CSdisc torque", "ELECTRON_VOLT_SI": "1.602176479703168341626628850680e-19", "Stellar derivative 69": "J direct impact gain", "Timestep multiplier 22": "CIRCUMBINARY_DISC", "Stellar derivative 64": "J CSdisc transfer", "System derivative 23": "J self-accretion RLOF loss", "Stellar derivative 66": "J CSdisc loss", "Stellar derivative 67": "J CSdisc L2 loss", "A_MERCURY_SI": "5.790000000000000000000000000000e+09", "System derivative 12": "J orbiting objects", "Timestep multiplier 37": "MINIMUM_TIMESTEP", "Stellar derivative 41": "Black-hole core mass", "System derivative 5": "J Wind Gain", "Stellar derivative 7": "M RLOF Loss", "Timestep multiplier 25": "FASTWIND", "Timestep multiplier 24": "DISC", "Timestep multiplier 4": "PREROCHE_HG", "Stellar derivative 33": "angular velocity (tides)", "ANSI colour 17 BRIGHT_BOLD : Default": "\u001b[1;1m[1;1m\u001b[0;0m.", "Timestep multiplier 16": "HeMS", "System derivative 15": "e Tides", "Timestep multiplier 52": "STELLAR_ANGMOM2", "BOLTZMANN_CONSTANT_SI": "1.380648519999999863079057996615e-23", "SPEED_OF_LIGHT_SI": "2.997924580000000000000000000000e+08", "STELLAR_POPULATIONS_ENSEMBLE_FILTER_NUMBER": "36", "Timestep multiplier 15": "TPAGB_NUCSYN_KARAKAS_SMOOTH", "Stellar derivative 58": "M CSdisc Loss via isotropic wind", "Stellar derivative 65": "J CSdisc gain", "ANSI colour 19 COLOUR_RESET : Default": "\u001b[0;0m[0;0m\u001b[0;0m.", "Stellar derivative 52": "Roche radius", "Stellar derivative 26": "J CBdisc gain", "PLANCK_CONSTANT_SI": "6.626075500000000021082466918401e-34", "Stellar derivative 35": "GB core mass", "Timestep multiplier 1": "MS", "ANSI colour 14 BRIGHT_MAGENTA : Default": "\u001b[1;35m[1;35m\u001b[0;0m.", "Timestep multiplier 27": "CEMP_POSTMS", "Timestep multiplier 28": "CEMP_NOTEMP", "Timestep multiplier 14": "TPAGB_NUCSYN_PREROCHE", "Timestep multiplier 36": "YVT", "Timestep multiplier 26": "SELMA", "Stellar derivative 1": "M Wind Loss", "Stellar derivative 43": "Central hydrogen", "Stellar derivative 31": "J (Total)", "L_SUN_SI": "3.851500000000000018329108480000e+26", "Timestep multiplier 21": "STELLAR_MAGNETIC_BRAKING", "Timestep multiplier 18": "OTHER_STELLAR_TYPES", "A_PLUTO_SI": "5.906400000000000000000000000000e+11", "R_SUN_SI": "6.956600000000000000000000000000e+08", "Stellar derivative 2": "M Wind Gain", "Stellar derivative 28": "J non-conservative", "Stellar derivative 44": "Central helium", "M_ELECTRON_SI": "9.109383000000000042603416415741e-31", "Stellar derivative 13": "M Disc Loss", "System derivative 30": "Jorbit stellar overspin gain", "Stellar derivative 0": "M (Total)", "STEFAN_BOLTZMANN_CONSTANT_SI": "5.670352798655924594054230964031e-08", "Timestep multiplier 38": "MAXIMUM_TIMESTEP", "MEGAPARSEC_SI": "3.085677581491367627980800000000e+22", "Stellar derivative 42": "Central temperature", "Stellar derivative 4": "Luminosity", "Stellar derivative 19": "J RLOF Loss", "FINE_STRUCTURE_CONSTANT_SI": "7.297345268281926408682203089029e-03", "Timestep multiplier 51": "ORBITAL_ANGMOM", "ANSI colour 5 BLUE : Default": "\u001b[0;34m[0;34m\u001b[0;0m.", "ANSI colour 1 RED : Default": "\u001b[0;31m[0;31m\u001b[0;0m.", "Stellar derivative 60": "J RLOF gain by self-accretion RLOF", "Stellar derivative 12": "M Disc Gain", "Timestep multiplier 2": "PREMS", "System derivative 14": "e Gravitational Radiation", "System derivative 3": "J Gravitational Radiation", "Stellar derivative 37": "ONe core mass", "ANSI colour 10 BRIGHT_RED : Default": "\u001b[1;31m[1;31m\u001b[0;0m.", "Float order": "little endian", "Stellar derivative 68": "J CSdisc isotropic loss", "Stellar derivative 18": "M artificial", "Stellar derivative 23": "J Tides", "Timestep multiplier 56": "GRAVITATIONAL_WAVE_RADIATION", "Stellar derivative 48": "Number of thermal pulses", "Stellar derivative 15": "M CBdisc Gain", "Timestep multiplier 35": "BLUE_STRAGGLER", "GRAVITATIONAL_CONSTANT_SI": "6.674080000000000335154563090628e-11", "A_NEPTUNE_SI": "4.495100000000000610351562500000e+11", "M_NEUTRON_SI": "1.674928999999999906378497198907e-27", "System derivative 21": "J stellar nonconservative", "Timestep multiplier 50": "MASSLESS_REMNANT", "KILOPARSEC_SI": "3.085677581491367600000000000000e+16", "Timestep multiplier 54": "MASS_GAIN2", "System derivative 28": "J CSdisc L2 mass loss", "Stellar derivative 30": "J core-envelope coupling", "Timestep multiplier 10": "EAGB_PREROCHE", "System derivative 8": "J Circumbinary Disc", "Stellar derivative 61": "J RLOF loss by self-accretion RLOF", "Timestep multiplier 6": "FGB", "Timestep multiplier 12": "TPAGB_NUCSYN_INTERPULSE", "PLANCK_CONSTANT_BAR_SI": "1.054572669125101842994825763174e-34", "System derivative 2": "e (total)", "Stellar derivative 56": "M CSdisc Loss", "PARSEC_SI": "3.085677581491367600000000000000e+16", "Timestep multiplier 60": "ZOOMFAC", "Stellar derivative 49": "Number of thermal pulses since mcmin", "Stellar derivative 38": "Si core mass", "uncaught": ["Wind MDOT_MS = 0", "Speed tests for 1 milliseconds", "NaN checker gives 0", "Random number mean 0.500021", "Binary_c/nucsyn by Robert Izzard, originally based on BSE of Hurley, Pols, Tout, Aarseth, but with many updates and rewrites.", "Wind MDOT_AGB = 2", "Compiled for 64 bit architecture", "Wind MDOT_GB = 1", "SVN revision unknown", "_SC_CLK_TCK = 100", "Comenv accretion:", "TRUE tests - should all give Yes : \"T\" = Yes, \"t\" = Yes, \"TRUE\" = Yes, \"True\" = Yes, \"true\" = Yes, \"truE\" = Yes, \"on\" = Yes, \"On\" = Yes, \"ON\" = Yes, \"1\" = Yes,", "Size of : short int 2, unsigned short int 2, int 4, unsigned int 4, long int 8, unsigned long int 8, long long int 8, unsigned long long int 8, size_t 8, float 4, double 8, long double 16, char 1, Boolean 1, stardata_t 175128, preferences_t 66400, star_t 6736, common_t 61312, model_t 100056, diffstats_t 256, probability_distribution_t 56, RLOF_orbit_t 40, store_t 2328, tmpstore_t 352, data_table_t 40, stardata_dump_t 1248384, GSL_args_t 40, envelope_t 168, envelope_shell_t 128, equation_of_state_t 248, opacity_t 80, kick_system_t 160, coordinate_t 24, binary_system_t 216, power_law_t 40, disc_thermal_zone_t 544, disc_loss_t 24, disc_t 3040, mersenne_twister_t 2504, binary_c_random_buffer_t 2520, binary_c_file_t 4144, difflogitem_t 40, difflogstack_t 24, binary_c_fixed_timestep_t 56, new_supernova_t 48, splitinfo_t 32, derivative_t 32, mint_t 112, orbit_t 64, Random_seed 8, Random_buffer 2504, FILE 216, void* 8, short int* 8, unsigned short int* 8, int* 8, unsigned int* 8, long int* 8, unsigned long int* 8, long long int* 8, unsigned long long int* 8, float* 8, double* 8, long double* 8, char* 8, Boolean* 8, stardata_t* 8, star_t* 8, FILE* 8, __int__ 4, __double__ 8, __unsigned__ __int__ 4, __short__ __int__ 4, __long__ __int__ 8, Hash_key_type 2, hash_entry_t 288 , disc_t 3040, disc_thermal_zone_t 544, power_law_t 40", "Wind MDOT_OTHER = 5", "Compiled in parameters:", "BACKTRACE_METHOD 3 GNU_BUFFER", "SVN URL unknown", "TRUE tests - should all give No : \"F\" = No, \"f\" = No, \"FALSE\" = No, \"False\" = No, \"falsE\" = No, \"off\" = No, \"Off\" = No, \"OFF\" = No, \"0\" = No, \"01\" = No, \"10\" = No, FALSE tests - should all give Yes : \"F\" = Yes, \"f\" = Yes, \"FALSE\" = Yes, \"False\" = Yes, \"falsE\" = Yes, \"off\" = Yes, \"Off\" = Yes, \"OFF\" = Yes, \"0\" = Yes, \"01\" = No, \"10\" = No,", "Wind MDOT_LBV = 4", "Wind MDOT_WR = 3", "Wind MDOT_COUNT = 6", "builtin_isnan gives 1", "Binary_c standard input units: \u00d7 these to get cgs", "Stack limit current = 18446744073709551615, max = 18446744073709551615 (-1 means no limit)"]}}, "binary_c_help_all": {"stars": {"section_name": "stars", "parameters": {"metallicity": {"param_name": "metallicity", "description": "This sets the metallicity of the stars, i.e. the amount (by mass) of matter which is not hydrogen or helium. If you are using the BSE algorithm, this must be 1e-4 <= metallicity <= 0.03. See also nucsyn_metallicity and effective_metallicity.", "rest": "(null)"}, "effective_metallicity": {"param_name": "effective_metallicity", "description": "This sets effective metallicity of stars as used in routines like the Schneider wind loss. If not set, or set to DEFAULT_TO_METALLICITY (==-1, the default), this is just the same as metallicity. The main difference between effective_metallicity and metallicity is the range of validity: 0 <= effective_metallicity <= 1, while metallicity's range of validity is limited by the stellar evolution algorithm (so, for BSE, is 1e-4 <= metallicity <= 0.03).", "rest": "(null)"}, "M_1": {"param_name": "M_1", "description": "The initial mass of star one (in solar units, internally this is star index 0).", "rest": "(null)"}, "M_2": {"param_name": "M_2", "description": "The initial mass of star two (in solar units, internally this is star index 1).", "rest": "(null)"}, "M_3": {"param_name": "M_3", "description": "The initial mass of star three (in solar units, internally this is star index 2).", "rest": "(null)"}, "M_4": {"param_name": "M_4", "description": "The initial mass of star four (in solar units, internally this is star index 3).", "rest": "(null)"}, "vrot1": {"param_name": "vrot1", "description": "The initial equatorial rotational velocity of star one (in km/s, internally this is star index 0). If 0.0, the Hurley et al 2000/2002 prescription is used to set the main-sequence velocity, so for a truly non-rotating star, set to something small (e.g. 0.001). See also vrot2,3,4.", "rest": "(null)"}, "vrot2": {"param_name": "vrot2", "description": "The initial equatorial rotational velocity of star two (in km/s, internally this is star index 1). If 0.0, the Hurley et al 2000/2002 prescription is used to set the main-sequence velocity, so for a truly non-rotating star, set to something small (e.g. 0.001). See also vrot1,3,4.", "rest": "(null)"}, "vrot3": {"param_name": "vrot3", "description": "The initial equatorial rotational velocity of star three (in km/s, internally this is star index 2). If 0.0, the Hurley et al 2000/2002 prescription is used to set the main-sequence velocity, so for a truly non-rotating star, set to something small (e.g. 0.001). See also vrot1,2,4.", "rest": "(null)"}, "vrot4": {"param_name": "vrot4", "description": "The initial equatorial rotational velocity of star four (in km/s, internally this is star index 3). If 0.0, the Hurley et al 2000/2002 prescription is used to set the main-sequence velocity, so for a truly non-rotating star, set to something small (e.g. 0.001). See also vrot1,2,3.", "rest": "(null)"}, "fKerr1": {"param_name": "fKerr1", "description": "Sets the angular momentum of star 1 to this fraction of the Kerr maximal angular momentum. Must be 0<=fKerr1<=1. See also fKerr2,3,4.", "rest": "(null)"}, "fKerr2": {"param_name": "fKerr2", "description": "Sets the angular momentum of star 2 to this fraction of the Kerr maximal angular momentum. Must be 0<=fKerr2<=1.  See also fKerr1,3,4.", "rest": "(null)"}, "fKerr3": {"param_name": "fKerr3", "description": "Sets the angular momentum of star 3 to this fraction of the Kerr maximal angular momentum. Must be 0<=fKerr3<=1. See also fKerr1,2,4.", "rest": "(null)"}, "fKerr4": {"param_name": "fKerr4", "description": "Sets the angular momentum of star 4 to this fraction of the Kerr maximal angular momentum. Must be 0<=fKerr4<=1.See also fKerr1,2,3.", "rest": "(null)"}, "vrot_multiplier1": {"param_name": "vrot_multiplier1", "description": "Multiplier for vrot1 or Prot1. Defaults to 1.0. Ignored if vrot1 > 0.0. See also vrot_multiplier2,3,4.", "rest": "(null)"}, "vrot_multiplier2": {"param_name": "vrot_multiplier2", "description": "Multiplier for vrot2 or Prot2. Defaults to 1.0. Ignored if vrot2 > 0.0. See also vrot_multiplier1,3,4.", "rest": "(null)"}, "vrot_multiplier3": {"param_name": "vrot_multiplier3", "description": "Multiplier for vrot3 or Prot3. Defaults to 1.0. Ignored if vrot3 > 0.0. See also vrot_multiplier1,2,4.", "rest": "(null)"}, "vrot_multiplier4": {"param_name": "vrot_multiplier4", "description": "Multiplier for vrot4 or Prot4. Defaults to 1.0. Ignored if vrot4 > 0.0. See also vrot_multiplier1,2,3.", "rest": "(null)"}, "Prot1": {"param_name": "Prot1", "description": "The initial equatorial rotational period of star one (in km/s, internally this is star index 0). See also Prot2,3,4.", "rest": "(null)"}, "Prot2": {"param_name": "Prot2", "description": "The initial equatorial rotational period of star two (in km/s, internally this is star index 1). See also Prot1,3,4.", "rest": "(null)"}, "Prot3": {"param_name": "Prot3", "description": "The initial equatorial rotational period of star three (in days, internally this is star index 2). See also Prot1,2,4.", "rest": "(null)"}, "Prot4": {"param_name": "Prot4", "description": "The initial equatorial rotational period of star four (in days, internally this is star index 3). See also Prot1,2,3.", "rest": "(null)"}, "inclination1": {"param_name": "inclination1", "description": "The initial inclination of star one (in degrees).", "rest": "(null)"}, "inclination2": {"param_name": "inclination2", "description": "The initial inclination of star two (in degrees).", "rest": "(null)"}, "inclination3": {"param_name": "inclination3", "description": "The initial inclination of star three (in degrees).", "rest": "(null)"}, "inclination4": {"param_name": "inclination4", "description": "The initial inclination of star four (in degrees).", "rest": "(null)"}, "B_1": {"param_name": "B_1", "description": "The initial magnetic field of star one (in Gauss, internally this is star index 0).", "rest": "(null)"}, "B_2": {"param_name": "B_2", "description": "The initial magnetic field of star two (in Gauss, internally this is star index 1).", "rest": "(null)"}, "B_3": {"param_name": "B_3", "description": "The initial magnetic field of star three (in Gauss, internally this is star index 2).", "rest": "(null)"}, "B_4": {"param_name": "B_4", "description": "The initial magnetic field of star four (in Gauss, internally this is star index 3).", "rest": "(null)"}, "B_inclination1": {"param_name": "B_inclination1", "description": "The initial inclination of the magnetic field of star one (in degrees).", "rest": "(null)"}, "B_inclination2": {"param_name": "B_inclination2", "description": "The initial inclination of the magnetic field of star two (in degrees).", "rest": "(null)"}, "B_inclination3": {"param_name": "B_inclination3", "description": "The initial inclination of the magnetic field of star three (in degrees).", "rest": "(null)"}, "B_inclination4": {"param_name": "B_inclination4", "description": "The initial inclination of the magnetic field of star four (in degrees).", "rest": "(null)"}, "stellar_type_1": {"param_name": "stellar_type_1", "description": "Set the stellar type of star 1 (internal index 0), usually MAIN_SEQUENCE (main sequence). Note that setting the stellar type only works for stars with both age=0 and core_mass=0, i.e. main sequence (hydrogen or helium), white dwarfs, black holes and neutrn stars.", "rest": "(null)"}, "stellar_type_2": {"param_name": "stellar_type_2", "description": "Set the stellar type of star 2 (internal index 1), usually MAIN_SEQUENCE (main sequence). Note that setting the stellar type only works for stars with both age=0 and core_mass=0, i.e. main sequence (hydrogen or helium), white dwarfs, black holes and neutrn stars.", "rest": "(null)"}, "stellar_type_3": {"param_name": "stellar_type_3", "description": "Set the stellar type of star 3 (internal index 2), usually MAIN_SEQUENCE (main sequence). Note that setting the stellar type only works for stars with both age=0 and core_mass=0, i.e. main sequence (hydrogen or helium), white dwarfs, black holes and neutrn stars.", "rest": "(null)"}, "stellar_type_4": {"param_name": "stellar_type_4", "description": "Set the stellar type of star 4 (internal index 3), usually MAIN_SEQUENCE (main sequence). Note that setting the stellar type only works for stars with both age=0 and core_mass=0, i.e. main sequence (hydrogen or helium), white dwarfs, black holes and neutrn stars.", "rest": "(null)"}, "max_stellar_type_1": {"param_name": "max_stellar_type_1", "description": "The maximum stellar type of star 1 (internal index 0). Evolution is stopped when the star reaches this stellar type. If this is negative, massless remnants are allowed, and the maximum stellar type is the absolute value. ", "rest": "(null)"}, "max_stellar_type_2": {"param_name": "max_stellar_type_2", "description": "The maximum stellar type of star 2 (internal index 1). Evolution is stopped when the star reaches this stellar type. If this is negative, massless remnants are allowed, and the maximum stellar type is the absolute value.", "rest": "(null)"}, "max_stellar_type_3": {"param_name": "max_stellar_type_3", "description": "The maximum stellar type of star 3 (internal index 2). Evolution is stopped when the star reaches this stellar type. If this is negative, massless remnants are allowed, and the maximum stellar type is the absolute value.", "rest": "(null)"}, "max_stellar_type_4": {"param_name": "max_stellar_type_4", "description": "The maximum stellar type of star 4 (internal index 3). Evolution is stopped when the star reaches this stellar type. If this is negative, massless remnants are allowed, and the maximum stellar type is the absolute value.", "rest": "(null)"}, "probability": {"param_name": "probability", "description": "The probability is a weighting applied to the star based on, say, the initial mass function. When running a grid of stars to simulate *all* stars, the summed probability of all the stars should be 1.0.", "rest": "(null)"}, "phasevol": {"param_name": "phasevol", "description": "The system's phase volume, used by binary_grid.", "rest": "(null)"}, "stellar_structure_algorithm": {"param_name": "stellar_structure_algorithm", "description": "Set the stellar structure algorithm. 0=modified BSE (default), 1=none, 2=external function (must be defined by the calling code), 3=binary_c (not yet implemented).", "rest": "(null)"}, "solver": {"param_name": "solver", "description": "The type of solver. Default is the Forward-Euler (0), but could be RK2 (1), RK4 (2) or a predictor-corretor (3).", "rest": "(null)"}, "max_evolution_time": {"param_name": "max_evolution_time", "description": "Set the maximum age for the stars (Myr).", "rest": "(null)"}, "max_model_number": {"param_name": "max_model_number", "description": "Set the maximum number of models, ignored if 0 (default is 0).", "rest": "(null)"}, "monte_carlo_kicks": {"param_name": "monte_carlo_kicks", "description": "Turn on Monte-Carlo SN kicks. On (True) by default, and indeed other algorithms are probably broken.", "rest": "(null)"}, "disable_debug": {"param_name": "disable_debug", "description": "Disables debug output. Only has an effect when DEBUG is 1, which probably requires a rebuild. Default FALSE.", "rest": "(null)"}, "debug_filter_pointers": {"param_name": "debug_filter_pointers", "description": "Filter pointers out of debug output, so that \"0x1234567\" becomes \"0xpointer\".", "rest": "(null)"}, "timestep_logging": {"param_name": "timestep_logging", "description": "Turn on timestep logging (default is False).", "rest": "(null)"}, "flush_log": {"param_name": "flush_log", "description": "Turn on flushing of the log file (default is False, which is faster).", "rest": "(null)"}, "derivative_logging": {"param_name": "derivative_logging", "description": "Turn on derivative logging (default is False).", "rest": "(null)"}, "progress_bar": {"param_name": "progress_bar", "description": "Turn on progress-bar logging (default is False).", "rest": "(null)"}, "log_all_reject_timestep_failures": {"param_name": "log_all_reject_timestep_failures", "description": "Turn on logging of every timestep that is rejected but which cannot have its timestep shortened.", "rest": "(null)"}, "cannot_shorten_timestep_policy": {"param_name": "cannot_shorten_timestep_policy", "description": "Turn on logging of every timestep that is rejected but which cannot have its timestep shortened.", "rest": "(null)"}, "rejects_in_log": {"param_name": "rejects_in_log", "description": "Show timestep rejections in the main log (default is False).", "rest": "(null)"}, "vandenHeuvel_logging": {"param_name": "vandenHeuvel_logging", "description": "Turn on van den Heuvel logging (default is False).", "rest": "(null)"}, "evolution_splitting": {"param_name": "evolution_splitting", "description": "If True, turn on splitting of an evolutionary run if splitpoint (e.g. supernova) occurs.", "rest": "(null)"}, "disable_events": {"param_name": "disable_events", "description": "Whether to disable the new events code (defaults to False, so we use events by default)", "rest": "(null)"}, "evolution_splitting_sn_eccentricity_threshold": {"param_name": "evolution_splitting_sn_eccentricity_threshold", "description": "Threshold eccentricity above which evolution splitting happens in a system with no SN kick. (0.01)", "rest": "(null)"}, "evolution_splitting_sn_n": {"param_name": "evolution_splitting_sn_n", "description": "Number of runs to split into when a SN occurs.", "rest": "(null)"}, "evolution_splitting_maxdepth": {"param_name": "evolution_splitting_maxdepth", "description": "Max number of splits in an evolutionary run.", "rest": "(null)"}, "equation_of_state_algorithm": {"param_name": "equation_of_state_algorithm", "description": "Set the equation of state algorithm. 0 = Paczynski.", "rest": "(null)"}, "opacity_algorithm": {"param_name": "opacity_algorithm", "description": "Set the opacity algorithm. 0 = Paczynski, 1 = Ferguson/Opal.", "rest": "(null)"}, "wind_mass_loss": {"param_name": "wind_mass_loss", "description": "Defines the algorithm used for stellar winds. 0 = none, 1 = Hurley et al. (2002), 2 = Schneider (2018).", "rest": "0"}, "gbwind": {"param_name": "gbwind", "description": "Wind prescription for first red giant branch stars.  0=Reimers (Hurley et al 2000/2002; choose gb_reimers_eta=0.5 for their mass loss rate), 1=Schroeder+Cuntz 2005 (set gb_reimers_eta=1.0 for their mass loss rate).", "rest": "(null)"}, "postagbwind": {"param_name": "postagbwind", "description": "Apply special post-(A)GB prescription. Default is POSTAGB_WIND_USE_GIANT which means we just use whatever is prescribed on the giant branch. Other options include: POSTAGB_WIND_NONE = 1 (no wind on the post (A)GB), POSTAGB_WIND_KRTICKA2020 = 2 which uses Krticka, Kub\u00e1t and Krtickov\u00e1 (2020, A&A 635, A173).", "rest": "(null)"}, "Teff_postAGB_min": {"param_name": "Teff_postAGB_min", "description": "The minimum temperature for which we apply post-(A)GB winds. See also Teff_postAGB_max. (6000 K)", "rest": "(null)"}, "Teff_postAGB_max": {"param_name": "Teff_postAGB_max", "description": "The maximum temperature for which we apply post-(A)GB winds. See also Teff_postAGB_min. (120000 K)", "rest": "(null)"}, "mattsson_Orich_tpagbwind": {"param_name": "mattsson_Orich_tpagbwind", "description": "Experimental: turns on Mattsson's TPAGB wind when the star is oxygen rich. Requires MATTSSON_MASS_LOSS.", "rest": "(null)"}, "magnetic_braking_factor": {"param_name": "magnetic_braking_factor", "description": "Multiplier for the magnetic braking angular momentum loss rate.", "rest": "(null)"}, "magnetic_braking_gamma": {"param_name": "magnetic_braking_gamma", "description": "gamma factor in Rappaport style magnetic braking expression.", "rest": "(null)"}, "magnetic_braking_algorithm": {"param_name": "magnetic_braking_algorithm", "description": "Algorithm for the magnetic braking angular momentum loss rate. 0 = Hurley et al. 2002, 1 = Andronov, Pinnsonneault and Sills 2003, 2 = Barnes and Kim 2010 ", "rest": "(null)"}, "helium_flash_mass_loss": {"param_name": "helium_flash_mass_loss", "description": "Mass to be lost at the helium flash.", "rest": "(null)"}, "gb_reimers_eta": {"param_name": "gb_reimers_eta", "description": "First red giant branch wind multiplication factor, cf. eta in Reimers' mass loss formula. (This multiplies the 4e-13 in Reimers' formula, or the 8e-14 in Schroeder and Cuntz.)", "rest": "(null)"}, "gbwindfac": {"param_name": "gbwindfac", "description": "Multiplier for the giant branch wind mass loss rate", "rest": "(null)"}, "tpagbwindfac": {"param_name": "tpagbwindfac", "description": "Multiplier for the TPAGB wind mass loss rate", "rest": "(null)"}, "eagbwindfac": {"param_name": "eagbwindfac", "description": "Multiplier for the EAGB wind mass loss rate", "rest": "(null)"}, "nieuwenhuijzen_windfac": {"param_name": "nieuwenhuijzen_windfac", "description": "Multiplier for the Nieuwenhuijzen & de Jager wind mass loss rate", "rest": "(null)"}, "tpagbwind": {"param_name": "tpagbwind", "description": "Wind prescription during the TPAGB. 0=Karakas 2002 (a modified Vassiliadis and Wood 1993), 1=Hurley et al 2000/2002 (Vassiliadis and Wood 1993), 2=Reimers, 3=Bloecker, 4=Van Loon,  5=Rob's C-wind (broken?), 6,7=Vassiliadis and Wood 1993 (Karakas,Hurley variants respectively) when C/O>1, 8=Mattsson, 9 = Goldman et al. (2017), 10 = Beasor et al. (2020).", "rest": "(null)"}, "eagbwind": {"param_name": "eagbwind", "description": "Wind prescription during the EAGB. 0=BSE (Hurley+2002, based on VW93), 1 = Goldman et al. (2017), 2 = Beasor et al. (2020).", "rest": "(null)"}, "wind_gas_to_dust_ratio": {"param_name": "wind_gas_to_dust_ratio", "description": "Gas to dust ratio used in wind calculations (e.g. Goldman et al. 2017). Typically 200 (Milky Way)-500 (Magellanic Clouds). Default is 200, approximately as in MW stars.", "rest": "(null)"}, "vwind_multiplier": {"param_name": "vwind_multiplier", "description": "Multiplier for the stellar wind velocity.", "rest": "(null)"}, "vwind_beta": {"param_name": "vwind_beta", "description": "Beta for stellar wind speed calculations, where vwind=sqrt(beta) * escape velocity. Default 0.125 (from BSE, Hurley et al. 2002). ", "rest": "(null)"}, "superwind_mira_switchon": {"param_name": "superwind_mira_switchon", "description": "In the Vassiliadis and Wood (1993) AGB wind prescription, the superwind is turned on at a given Mira period, usually 500 days. You can vary when this switch-on happens with this parameter.", "rest": "(null)"}, "vw93_mira_shift": {"param_name": "vw93_mira_shift", "description": "In the Vassiliadis and Wood (1993) AGB wind prescription, the wind loss rate depends on the Mira period plus this offset. Requires VW93_MIRA_SHIFT.", "rest": "(null)"}, "vw93_multiplier": {"param_name": "vw93_multiplier", "description": "In the Vassiliadis and Wood (1993) AGB wind prescription, the wind loss rate is multiplied by this factor. Requires VW93_MULTIPLIER.", "rest": "(null)"}, "tpagb_reimers_eta": {"param_name": "tpagb_reimers_eta", "description": "TPAGB Reimers wind multiplication factor, cf. eta in Reimers' mass loss formula. (This multiplies the 4e-13 in Reimers' formula, or the 8e-14 in Schroeder and Cuntz.) Note that Reimers is not the default TPAGB wind prescription. See also tpagbwind.", "rest": "(null)"}, "Tout_Pringle_1992_multiplier": {"param_name": "Tout_Pringle_1992_multiplier", "description": "Multiplier for the Tout & Pringle (1992) magnetic wind. (0.0)", "rest": "(null)"}, "artificial_mass_accretion_rate%d": {"param_name": "artificial_mass_accretion_rate%d", "description": "Constant mass accretion rate for star <n>.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_type%d": {"param_name": "artificial_mass_accretion_rate_by_stellar_type%d", "description": "Constant mass accretion rate for stellar type <n>.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeLOW_MASS_MS": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeLOW_MASS_MS", "description": "Constant mass accretion rate for stellar type LOW_MASS_MS.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeMS": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeMS", "description": "Constant mass accretion rate for stellar type MS.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeHG": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeHG", "description": "Constant mass accretion rate for stellar type HG.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeGIANT_BRANCH": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeGIANT_BRANCH", "description": "Constant mass accretion rate for stellar type GIANT_BRANCH.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeCHeB": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeCHeB", "description": "Constant mass accretion rate for stellar type CHeB.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeEAGB": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeEAGB", "description": "Constant mass accretion rate for stellar type EAGB.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeTPAGB": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeTPAGB", "description": "Constant mass accretion rate for stellar type TPAGB.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeHeMS": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeHeMS", "description": "Constant mass accretion rate for stellar type HeMS.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeHeHG": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeHeHG", "description": "Constant mass accretion rate for stellar type HeHG.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeHeGB": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeHeGB", "description": "Constant mass accretion rate for stellar type HeGB.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeHeWD": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeHeWD", "description": "Constant mass accretion rate for stellar type HeWD.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeCOWD": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeCOWD", "description": "Constant mass accretion rate for stellar type COWD.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeONeWD": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeONeWD", "description": "Constant mass accretion rate for stellar type ONeWD.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeNS": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeNS", "description": "Constant mass accretion rate for stellar type NS.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeBH": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeBH", "description": "Constant mass accretion rate for stellar type BH.", "rest": "(null)"}, "artificial_mass_accretion_rate_by_stellar_typeMASSLESS_REMNANT": {"param_name": "artificial_mass_accretion_rate_by_stellar_typeMASSLESS_REMNANT", "description": "Constant mass accretion rate for stellar type MASSLESS_REMNANT.", "rest": "(null)"}, "artificial_angular_momentum_accretion_rate%d": {"param_name": "artificial_angular_momentum_accretion_rate%d", "description": "Constant angular momentum accretion for star <n>.", "rest": "(null)"}, "artificial_orbital_angular_momentum_accretion_rate": {"param_name": "artificial_orbital_angular_momentum_accretion_rate", "description": "Constant angular momentum accretion rate on the orbit.", "rest": "(null)"}, "artificial_accretion_start_time": {"param_name": "artificial_accretion_start_time", "description": "Time at which artificial accretion stars. Ignored if <0 (default is -1).", "rest": "(null)"}, "artificial_accretion_end_time": {"param_name": "artificial_accretion_end_time", "description": "Time at which artificial accretion ends. Ignored if <0 (default is -1).", "rest": "(null)"}, "wr_wind": {"param_name": "wr_wind", "description": "Massive-star (WR) wind prescription. 0 = Hurley et al 2000/2002, 1=Maeder and Meynet, 2=Nugis and Lamers, 3=John Eldridge's version of Vink's early-2000s wind (See Lynnette Dray's thesis, or John Eldridge's thesis)", "rest": "(null)"}, "wr_wind_fac": {"param_name": "wr_wind_fac", "description": "Massive-star (WR) wind multiplication factor.", "rest": "(null)"}, "wrwindfac": {"param_name": "wrwindfac", "description": "Massive-star (WR) wind multiplication factor. Synonymous with wr_wind_fac (which you should use instead).", "rest": "(null)"}, "BH_prescription": {"param_name": "BH_prescription", "description": "Black hole mass prescrition: relates the mass of a newly formed black hole to its progenitor's (CO) core mass. BH_HURLEY2002 = 0 = Hurley et al 2000/2002, BH_BELCZYNSKI = 1 = Belczynski (early 2000s), BH_SPERA2015 = Spera+ 2015, BH_FRYER12_DELAYED = 3 = Fryer et al. (2012) delayed prescription, BH_FRYER12_RAPID = 4 = Fryer et al. (2012) rapid prescription, BH_FRYER12_STARTRACK = 5 = Fryer et al. (2012) startrack prescription, BH_DARK = 6 = set BH mass to the CO core mass so no mass is ejected, BH_MARASSI2019 = 7 use Marassi 2019 prescription.", "rest": "(null)"}, "sn_kick_distribution_II": {"param_name": "sn_kick_distribution_II", "description": "Set the distribution of speeds applied to kick type II core collapse supernova systems. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_ECAP": {"param_name": "sn_kick_distribution_ECAP", "description": "Set the distribution of speeds applied to the remnants of electron-capture supernovae. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_NS_NS": {"param_name": "sn_kick_distribution_NS_NS", "description": "Set the distribution of speeds applied to kick neutron stars and black holes that survive a NS-NS merger. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_IBC": {"param_name": "sn_kick_distribution_IBC", "description": "Set the distribution of speeds applied to kick newly-born neutron stars and black holes after a type Ib/c core-collapse supernova. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_GRB_COLLAPSAR": {"param_name": "sn_kick_distribution_GRB_COLLAPSAR", "description": "Set the distribution of speeds applied to kick newly-born neutron stars and black holes after a type Ib/c core-collapse supernova which is also a collapsar. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_TZ": {"param_name": "sn_kick_distribution_TZ", "description": "Set the distribution of speeds applied to kick newly-born neutron stars and black holes at the death of a Thorne-Zytkow object. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_AIC_BH": {"param_name": "sn_kick_distribution_AIC_BH", "description": "Set the distribution of speeds applied to kick newly-born neutron stars black holes after accretion induced collapse of a neutron star. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_BH_BH": {"param_name": "sn_kick_distribution_BH_BH", "description": "Set the distribution of speeds applied to black holes formed by the merger of two black holes. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_BH_NS": {"param_name": "sn_kick_distribution_BH_NS", "description": "Set the distribution of speeds applied to black holes formed by the merger of a neutron star and a black holes. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_IA_Hybrid_HeCOWD": {"param_name": "sn_kick_distribution_IA_Hybrid_HeCOWD", "description": "Set the distribution of speeds applied to any survivor of a hybrid He-COWD SNIa explosion. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_distribution_IA_Hybrid_HeCOWD_subluminous": {"param_name": "sn_kick_distribution_IA_Hybrid_HeCOWD_subluminous", "description": "Set the distribution of speeds applied to any survivor of a subluminous hybrid He-COWD SNIa explosion. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_II": {"param_name": "sn_kick_dispersion_II", "description": "Set the dispersion of speeds applied to kick type II core collapse supernova systems. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_ECAP": {"param_name": "sn_kick_dispersion_ECAP", "description": "Set the dispersion of speeds applied to the remnants of electron-capture supernovae. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_NS_NS": {"param_name": "sn_kick_dispersion_NS_NS", "description": "Set the dispersion of speeds applied to kick neutron stars and black holes that survive a NS-NS merger. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_IBC": {"param_name": "sn_kick_dispersion_IBC", "description": "Set the dispersion of speeds applied to kick newly-born neutron stars and black holes after a type Ib/c core-collapse supernova. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_GRB_COLLAPSAR": {"param_name": "sn_kick_dispersion_GRB_COLLAPSAR", "description": "Set the dispersion of speeds applied to kick newly-born neutron stars and black holes after a type Ib/c core-collapse supernova which is also a collapsar. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_TZ": {"param_name": "sn_kick_dispersion_TZ", "description": "Set the dispersion of speeds applied to kick newly-born neutron stars and black holes at the death of a Thorne-Zytkow object. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_AIC_BH": {"param_name": "sn_kick_dispersion_AIC_BH", "description": "Set the dispersion of speeds applied to kick newly-born neutron stars black holes after accretion induced collapse of a neutron star. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_BH_BH": {"param_name": "sn_kick_dispersion_BH_BH", "description": "Set the dispersion of speeds applied to black holes formed by the merger of two black holes. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_BH_NS": {"param_name": "sn_kick_dispersion_BH_NS", "description": "Set the dispersion of speeds applied to black holes formed by the merger of a neutron star and a black holes. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_IA_Hybrid_HeCOWD": {"param_name": "sn_kick_dispersion_IA_Hybrid_HeCOWD", "description": "Set the dispersion of speeds applied to the survivor of a SNIa explosion of a hybrid He-COWD. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_dispersion_IA_Hybrid_HeCOWD_subluminous": {"param_name": "sn_kick_dispersion_IA_Hybrid_HeCOWD_subluminous", "description": "Set the dispersion of speeds applied to the survivor of a subluminous SNIa explosion of a hybrid He-COWD. 0=fixed, 1=maxwellian (hurley/BSE), 2=custom function (see monte_carlo_kicks.c).", "rest": "(null)"}, "sn_kick_companion_IA_He": {"param_name": "sn_kick_companion_IA_He", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a Ia He supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IA_ELD": {"param_name": "sn_kick_companion_IA_ELD", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a Ia ELD (sub-Mch) supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IA_CHAND": {"param_name": "sn_kick_companion_IA_CHAND", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a Ia Mch supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_AIC": {"param_name": "sn_kick_companion_AIC", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when an accretion induced collapse (supernova) occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_ECAP": {"param_name": "sn_kick_companion_ECAP", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when an electron capture supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IA_He_Coal": {"param_name": "sn_kick_companion_IA_He_Coal", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a Ia helium merger supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IA_CHAND_Coal": {"param_name": "sn_kick_companion_IA_CHAND_Coal", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a Ia Mch merger supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_NS_NS": {"param_name": "sn_kick_companion_NS_NS", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a neutron-star neutron-star merger. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_GRB_COLLAPSAR": {"param_name": "sn_kick_companion_GRB_COLLAPSAR", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a GRB Collapsar (rapidly rotating SN Ibc) supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_HeStarIa": {"param_name": "sn_kick_companion_HeStarIa", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a He-star Ia supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IBC": {"param_name": "sn_kick_companion_IBC", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a type Ib/c supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_II": {"param_name": "sn_kick_companion_II", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a type II supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IIa": {"param_name": "sn_kick_companion_IIa", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a type IIa supernova occurs. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_WDKICK": {"param_name": "sn_kick_companion_WDKICK", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a WD is kicked. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_TZ": {"param_name": "sn_kick_companion_TZ", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a Thorne-Zytkow object is formed. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_AIC_BH": {"param_name": "sn_kick_companion_AIC_BH", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a neutron star collapses to a black hole. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_BH_BH": {"param_name": "sn_kick_companion_BH_BH", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when two black holes merge. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_BH_NS": {"param_name": "sn_kick_companion_BH_NS", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the, kick on the companion when a black hole merges with a neutron star. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IA_Hybrid_HeCOWD": {"param_name": "sn_kick_companion_IA_Hybrid_HeCOWD", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the kick on the companion, if it survives, in a hybrid He-COWD type Ia explosion. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "sn_kick_companion_IA_Hybrid_HeCOWD_subluminous": {"param_name": "sn_kick_companion_IA_Hybrid_HeCOWD_subluminous", "description": "Set the speed (if >=0) of, or the algothim (if <0) used to calculate the kick on the companion, if it survives, in a subluminous hybrid He-COWD type Ia explosion. 0 = none, 1 = Liu+2015, 2 = Wheeler+ 1975.", "rest": "(null)"}, "wd_sigma": {"param_name": "wd_sigma", "description": "Set the speed at which white dwarfs are kicked when they form, in km/s. Default is zero (i.e. no kick). Requires WD_KICKS.", "rest": "(null)"}, "wd_kick_direction": {"param_name": "wd_kick_direction", "description": "Set the direction of white dwarf kicks. 0 = random, 1 = up, 2 = forward, 3 = backward, 4 = inward, 5 = outward. Requires WD_KICKS.", "rest": "(null)"}, "wd_kick_when": {"param_name": "wd_kick_when", "description": "Decide when to kick a white dwarf. 0=at birth, 1=at first RLOF, 2=at given pulse number (see wd_kick_pulse_number), 3 at every pulse Requires WD_KICKS.", "rest": "(null)"}, "wd_kick_pulse_number": {"param_name": "wd_kick_pulse_number", "description": "Apply a kick to a star at a desired pulse number on the TPAGB (i.e. pre-WD). Requires WD_KICKS.", "rest": "(null)"}, "minimum_helium_ignition_core_mass": {"param_name": "minimum_helium_ignition_core_mass", "description": "Minimum helium core mass required to ignite helium in the case that the hydrogen envelope is stripped on the giant branch, e.g. to make an sdB or sdO star. Typically 0.4, if 0.0 then the BSE algorithm (based on the total mass) is used.", "rest": "(null)"}, "minimum_CO_core_mass_for_carbon_ignition": {"param_name": "minimum_CO_core_mass_for_carbon_ignition", "description": "Minimum CO core mass for carbon ignition, assuming Mc,bagb>1.6Msun. Typically around 1.08Msun (Pols+1998).", "rest": "(null)"}, "minimum_CO_core_mass_for_neon_ignition": {"param_name": "minimum_CO_core_mass_for_neon_ignition", "description": "Minimum CO core mass for neon ignition. Typically around 1.42Msun. Stars that have cores that ignite carbon, but not neon explode in electon-capture supernovae.", "rest": "(null)"}, "minimum_mcbagb_for_nondegenerate_carbon_ignition": {"param_name": "minimum_mcbagb_for_nondegenerate_carbon_ignition", "description": "Minimum Mc,bagb (core mass at the base of the AGB) for non-degenerate carbon ignition. Typically around 2.25Msun (Pols+1998).", "rest": "(null)"}, "maximum_mcbagb_for_degenerate_carbon_ignition": {"param_name": "maximum_mcbagb_for_degenerate_carbon_ignition", "description": "Maximum Mc,bagb (core mass at the base of the AGB) for degenerate carbon ignition. Typically around 1.6Msun (Pols+1998).", "rest": "(null)"}, "max_neutron_star_mass": {"param_name": "max_neutron_star_mass", "description": "Maximum mass of a neutron star before it collapses to a black hole. Typically around 2Msun.", "rest": "(null)"}, "chandrasekhar_mass": {"param_name": "chandrasekhar_mass", "description": "The Chandrasekhar mass, usually 1.44Msun", "rest": "(null)"}, "delta_mcmin": {"param_name": "delta_mcmin", "description": "A parameter to reduce the minimum core mass for third dredge up to occur on the TPAGB. As used by Izzard and Tout (2004) to increase the amount of dredge up, hence carbon, in Magellanic cloud stars.", "rest": "(null)"}, "lambda_min": {"param_name": "lambda_min", "description": "A parameter to increase the efficiency of third dredge up on the TPAGB. The efficiency is lambda * lambda_mult, and setting lambda_min>0 implies that, once Mc>Mcmin (see delta_mcmin) lambda=Max(lambda(fit to Karakas), lambda_min). As used by Izzard and Tout (2004) to increase the amount of dredge up, hence carbon, in Magellanic cloud stars. You can set this to THIRD_DREDGE_UP_LAMBDA_MIN_AUTO to match the results of Izzard and Tout (2004). See also lambda_multiplier.", "rest": "(null)"}, "lambda_multiplier": {"param_name": "lambda_multiplier", "description": "A parameter to increase the efficiency of third dredge up on the TPAGB. The efficiency is lambda * lambda_mult, and setting lambda_min>0 implies that, once Mc>Mcmin (see delta_mcmin) lambda=Max(lambda(fit to Karakas), lambda_min). As used by Izzard and Tout (2004) to increase the amount of dredge up, hence carbon, in Magellanic cloud stars.", "rest": "(null)"}, "minimum_envelope_mass_for_third_dredgeup": {"param_name": "minimum_envelope_mass_for_third_dredgeup", "description": "The minimum envelope mass for third dredge up on the TPAGB. Early, solar metallicity models by Straniero et al suggested 0.5Msun is typical. However, circumstantial evidence (Izzard et al 2009) as well as newer models by Stancliffe and Karakas suggest that at low metallicity a value nearer zero is more appropriate.", "rest": "(null)"}, "mass_of_pmz": {"param_name": "mass_of_pmz", "description": "The mass in the partial mixing zone of a TPAGB star, using the Karakas 2012 tables. Ask Carlo Abate for more details, or see the series of papers Abate et al 2012, 2013, 2014. Requires NUCSYN and USE_TABULAR_INTERSHELL_ABUNDANCES_KARAKAS_2012.", "rest": "(null)"}, "c13_eff": {"param_name": "c13_eff", "description": "The \"efficiency\" of partial mixing in a TPAGB star intershell region, when using the s-process tables of Gallino, Busso, Lugaro et al. as provided by Maria Lugaro for the Izzard et al. 2009 paper. Requires NUCSYN and NUCSYN_S_PROCESS.", "rest": "(null)"}, "mc13_pocket_multiplier": {"param_name": "mc13_pocket_multiplier", "description": "Multiplies the mass in the partial mixing zone of a TPAGB star, when using the s-process tables of Gallino, Busso, Lugaro et al. as provided by Maria Lugaro for the Izzard et al. 2009 paper. Requires NUCSYN and NUCSYN_S_PROCESS.", "rest": "(null)"}, "tides_convective_damping": {"param_name": "tides_convective_damping", "description": "Tidal convective damping algorithm. 0=TIDES_HURLEY2002 Zahn 197x timescales + Hut, as in Hurley et al (2002), 1 = TIDES_ZAHN1989: Zahn 1989 lambdas + Hut.", "rest": "(null)"}, "E2_prescription": {"param_name": "E2_prescription", "description": "Choose how to calculate the E2 structural parameter (used in tidal timescale calculations). 0=Hurley 1=Izzard (see Siess et al 2013).", "rest": "(null)"}, "dtfac": {"param_name": "dtfac", "description": "A parameter to decrease the timestep ONLY during the TPAGB phase.", "rest": "(null)"}, "hbbtfac": {"param_name": "hbbtfac", "description": "A parameter to modulate the temperature at the base of the hot-bottom burning zone in TPAGB stars. (Works only if NUCSYN is defined)", "rest": "(null)"}, "wind_multiplier_%d": {"param_name": "wind_multiplier_%d", "description": "Wind multiplier for the stellar type specified by the intger %d. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_LOW_MASS_MS": {"param_name": "wind_multiplier_LOW_MASS_MS", "description": "Wind multiplier for the stellar type specified by the intger -1919311099. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_MS": {"param_name": "wind_multiplier_MS", "description": "Wind multiplier for the stellar type specified by the intger -1919318169. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_HG": {"param_name": "wind_multiplier_HG", "description": "Wind multiplier for the stellar type specified by the intger -1919318136. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_GIANT_BRANCH": {"param_name": "wind_multiplier_GIANT_BRANCH", "description": "Wind multiplier for the stellar type specified by the intger -1919311087. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_CHeB": {"param_name": "wind_multiplier_CHeB", "description": "Wind multiplier for the stellar type specified by the intger -1919318129. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_EAGB": {"param_name": "wind_multiplier_EAGB", "description": "Wind multiplier for the stellar type specified by the intger -1919318124. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_TPAGB": {"param_name": "wind_multiplier_TPAGB", "description": "Wind multiplier for the stellar type specified by the intger -1919318095. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_HeMS": {"param_name": "wind_multiplier_HeMS", "description": "Wind multiplier for the stellar type specified by the intger -1919317994. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_HeHG": {"param_name": "wind_multiplier_HeHG", "description": "Wind multiplier for the stellar type specified by the intger -1919311074. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_HeGB": {"param_name": "wind_multiplier_HeGB", "description": "Wind multiplier for the stellar type specified by the intger -1919311069. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_HeWD": {"param_name": "wind_multiplier_HeWD", "description": "Wind multiplier for the stellar type specified by the intger -1919311064. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_COWD": {"param_name": "wind_multiplier_COWD", "description": "Wind multiplier for the stellar type specified by the intger -1919311059. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_ONeWD": {"param_name": "wind_multiplier_ONeWD", "description": "Wind multiplier for the stellar type specified by the intger -1919311054. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_NS": {"param_name": "wind_multiplier_NS", "description": "Wind multiplier for the stellar type specified by the intger -1919318929. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_BH": {"param_name": "wind_multiplier_BH", "description": "Wind multiplier for the stellar type specified by the intger -1919311048. By default these are all 1.0.", "rest": "(null)"}, "wind_multiplier_MASSLESS_REMNANT": {"param_name": "wind_multiplier_MASSLESS_REMNANT", "description": "Wind multiplier for the stellar type specified by the intger -1919317562. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_%d": {"param_name": "wind_type_multiplier_%d", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer %d. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_LOW_MASS_MS": {"param_name": "wind_type_multiplier_LOW_MASS_MS", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311099. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_MS": {"param_name": "wind_type_multiplier_MS", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919318169. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_HG": {"param_name": "wind_type_multiplier_HG", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919318136. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_GIANT_BRANCH": {"param_name": "wind_type_multiplier_GIANT_BRANCH", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311087. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_CHeB": {"param_name": "wind_type_multiplier_CHeB", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919318129. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_EAGB": {"param_name": "wind_type_multiplier_EAGB", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919318124. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_TPAGB": {"param_name": "wind_type_multiplier_TPAGB", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919318095. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_HeMS": {"param_name": "wind_type_multiplier_HeMS", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919317994. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_HeHG": {"param_name": "wind_type_multiplier_HeHG", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311074. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_HeGB": {"param_name": "wind_type_multiplier_HeGB", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311069. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_HeWD": {"param_name": "wind_type_multiplier_HeWD", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311064. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_COWD": {"param_name": "wind_type_multiplier_COWD", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311059. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_ONeWD": {"param_name": "wind_type_multiplier_ONeWD", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311054. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_NS": {"param_name": "wind_type_multiplier_NS", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919318929. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_BH": {"param_name": "wind_type_multiplier_BH", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919311048. By default these are all 1.0.", "rest": "(null)"}, "wind_type_multiplier_MASSLESS_REMNANT": {"param_name": "wind_type_multiplier_MASSLESS_REMNANT", "description": "Wind multiplier for different types of wind (MS, GB, AGB, WR, LBV, OTHER), given by the integer -1919317562. By default these are all 1.0.", "rest": "(null)"}, "pre_main_sequence": {"param_name": "pre_main_sequence", "description": "Set to True to turn on pre-main sequence evolution. Currently this is not a special stellar type, rather the first (small) fraction of the main sequence has increased radii to match the Railton et al 2014 fits to Tout's pre-main sequence stars. Requires PRE_MAIN_SEQUENCE. See also pre_main_sequence_fit_lobes.", "rest": "(null)"}, "pre_main_sequence_fit_lobes": {"param_name": "pre_main_sequence_fit_lobes", "description": "Set to True force a pre-main sequence star into its Roche lobe. This is done by artificially aging it. Requires PRE_MAIN_SEQUENCE", "rest": "(null)"}, "small_envelope_method": {"param_name": "small_envelope_method", "description": "Choose the method used to determine the stellar radius when the envelope mass is very thin. 0 = Hurley et al. (2002), 1 = Miller Bertolami et al. (2016+) for GB and AGB stars only.", "rest": "(null)"}, "timestep_modulator": {"param_name": "timestep_modulator", "description": "Multiplier applied to the global timestep. Requires TIMESTEP_MODULATION.", "rest": "(null)"}, "timestep_multiplier%d": {"param_name": "timestep_multiplier%d", "description": "Multiplier applied to timestep limit <n>.", "rest": "(null)"}, "timestep_multiplierNONE": {"param_name": "timestep_multiplierNONE", "description": "Multiplier applied to timestep limit NONE.", "rest": "(null)"}, "timestep_multiplierMS": {"param_name": "timestep_multiplierMS", "description": "Multiplier applied to timestep limit MS.", "rest": "(null)"}, "timestep_multiplierPREMS": {"param_name": "timestep_multiplierPREMS", "description": "Multiplier applied to timestep limit PREMS.", "rest": "(null)"}, "timestep_multiplierPREROCHE_MS": {"param_name": "timestep_multiplierPREROCHE_MS", "description": "Multiplier applied to timestep limit PREROCHE_MS.", "rest": "(null)"}, "timestep_multiplierPREROCHE_HG": {"param_name": "timestep_multiplierPREROCHE_HG", "description": "Multiplier applied to timestep limit PREROCHE_HG.", "rest": "(null)"}, "timestep_multiplierHG": {"param_name": "timestep_multiplierHG", "description": "Multiplier applied to timestep limit HG.", "rest": "(null)"}, "timestep_multiplierFGB": {"param_name": "timestep_multiplierFGB", "description": "Multiplier applied to timestep limit FGB.", "rest": "(null)"}, "timestep_multiplierCHeB": {"param_name": "timestep_multiplierCHeB", "description": "Multiplier applied to timestep limit CHeB.", "rest": "(null)"}, "timestep_multiplierEAGB": {"param_name": "timestep_multiplierEAGB", "description": "Multiplier applied to timestep limit EAGB.", "rest": "(null)"}, "timestep_multiplierEAGB_AXEL": {"param_name": "timestep_multiplierEAGB_AXEL", "description": "Multiplier applied to timestep limit EAGB_AXEL.", "rest": "(null)"}, "timestep_multiplierEAGB_PREROCHE": {"param_name": "timestep_multiplierEAGB_PREROCHE", "description": "Multiplier applied to timestep limit EAGB_PREROCHE.", "rest": "(null)"}, "timestep_multiplierTPAGB": {"param_name": "timestep_multiplierTPAGB", "description": "Multiplier applied to timestep limit TPAGB.", "rest": "(null)"}, "timestep_multiplierTPAGB_NUCSYN_INTERPULSE": {"param_name": "timestep_multiplierTPAGB_NUCSYN_INTERPULSE", "description": "Multiplier applied to timestep limit TPAGB_NUCSYN_INTERPULSE.", "rest": "(null)"}, "timestep_multiplierTPAGB_NUCSYN_SPEEDUP": {"param_name": "timestep_multiplierTPAGB_NUCSYN_SPEEDUP", "description": "Multiplier applied to timestep limit TPAGB_NUCSYN_SPEEDUP.", "rest": "(null)"}, "timestep_multiplierTPAGB_NUCSYN_PREROCHE": {"param_name": "timestep_multiplierTPAGB_NUCSYN_PREROCHE", "description": "Multiplier applied to timestep limit TPAGB_NUCSYN_PREROCHE.", "rest": "(null)"}, "timestep_multiplierTPAGB_NUCSYN_KARAKAS_SMOOTH": {"param_name": "timestep_multiplierTPAGB_NUCSYN_KARAKAS_SMOOTH", "description": "Multiplier applied to timestep limit TPAGB_NUCSYN_KARAKAS_SMOOTH.", "rest": "(null)"}, "timestep_multiplierHeMS": {"param_name": "timestep_multiplierHeMS", "description": "Multiplier applied to timestep limit HeMS.", "rest": "(null)"}, "timestep_multiplierHeHG_GB": {"param_name": "timestep_multiplierHeHG_GB", "description": "Multiplier applied to timestep limit HeHG_GB.", "rest": "(null)"}, "timestep_multiplierOTHER_STELLAR_TYPES": {"param_name": "timestep_multiplierOTHER_STELLAR_TYPES", "description": "Multiplier applied to timestep limit OTHER_STELLAR_TYPES.", "rest": "(null)"}, "timestep_multiplierSTELLAR_ANGMOM": {"param_name": "timestep_multiplierSTELLAR_ANGMOM", "description": "Multiplier applied to timestep limit STELLAR_ANGMOM.", "rest": "(null)"}, "timestep_multiplierSTELLAR_MASS_LOSS": {"param_name": "timestep_multiplierSTELLAR_MASS_LOSS", "description": "Multiplier applied to timestep limit STELLAR_MASS_LOSS.", "rest": "(null)"}, "timestep_multiplierSTELLAR_MAGNETIC_BRAKING": {"param_name": "timestep_multiplierSTELLAR_MAGNETIC_BRAKING", "description": "Multiplier applied to timestep limit STELLAR_MAGNETIC_BRAKING.", "rest": "(null)"}, "timestep_multiplierCIRCUMBINARY_DISC": {"param_name": "timestep_multiplierCIRCUMBINARY_DISC", "description": "Multiplier applied to timestep limit CIRCUMBINARY_DISC.", "rest": "(null)"}, "timestep_multiplier": {"param_name": "timestep_multiplier", "description": "Multiplier applied to timestep limit .", "rest": "(null)"}, "timestep_multiplierDISC": {"param_name": "timestep_multiplierDISC", "description": "Multiplier applied to timestep limit DISC.", "rest": "(null)"}, "timestep_multiplierFASTWIND": {"param_name": "timestep_multiplierFASTWIND", "description": "Multiplier applied to timestep limit FASTWIND.", "rest": "(null)"}, "timestep_multiplierSELMA": {"param_name": "timestep_multiplierSELMA", "description": "Multiplier applied to timestep limit SELMA.", "rest": "(null)"}, "timestep_multiplierCEMP_POSTMS": {"param_name": "timestep_multiplierCEMP_POSTMS", "description": "Multiplier applied to timestep limit CEMP_POSTMS.", "rest": "(null)"}, "timestep_multiplierCEMP_NOTEMP": {"param_name": "timestep_multiplierCEMP_NOTEMP", "description": "Multiplier applied to timestep limit CEMP_NOTEMP.", "rest": "(null)"}, "timestep_multiplierCEMP_EMP": {"param_name": "timestep_multiplierCEMP_EMP", "description": "Multiplier applied to timestep limit CEMP_EMP.", "rest": "(null)"}, "timestep_multiplierCEMP_NEARLY": {"param_name": "timestep_multiplierCEMP_NEARLY", "description": "Multiplier applied to timestep limit CEMP_NEARLY.", "rest": "(null)"}, "timestep_multiplierCEMP_FLOOR": {"param_name": "timestep_multiplierCEMP_FLOOR", "description": "Multiplier applied to timestep limit CEMP_FLOOR.", "rest": "(null)"}, "timestep_multiplierFABIAN_IMF_LOG": {"param_name": "timestep_multiplierFABIAN_IMF_LOG", "description": "Multiplier applied to timestep limit FABIAN_IMF_LOG.", "rest": "(null)"}, "timestep_multiplierHRD1": {"param_name": "timestep_multiplierHRD1", "description": "Multiplier applied to timestep limit HRD1.", "rest": "(null)"}, "timestep_multiplierHRD2": {"param_name": "timestep_multiplierHRD2", "description": "Multiplier applied to timestep limit HRD2.", "rest": "(null)"}, "timestep_multiplier16": {"param_name": "timestep_multiplier16", "description": "Multiplier applied to timestep limit 16.", "rest": "(null)"}, "timestep_multiplierYVT": {"param_name": "timestep_multiplierYVT", "description": "Multiplier applied to timestep limit YVT.", "rest": "(null)"}, "timestep_multiplierMINIMUM_TIMESTEP": {"param_name": "timestep_multiplierMINIMUM_TIMESTEP", "description": "Multiplier applied to timestep limit MINIMUM_TIMESTEP.", "rest": "(null)"}, "timestep_multiplierMAXIMUM_TIMESTEP": {"param_name": "timestep_multiplierMAXIMUM_TIMESTEP", "description": "Multiplier applied to timestep limit MAXIMUM_TIMESTEP.", "rest": "(null)"}, "timestep_multiplierMAXIMUM_TIMESTEP_BY_STELLAR_TYPE": {"param_name": "timestep_multiplierMAXIMUM_TIMESTEP_BY_STELLAR_TYPE", "description": "Multiplier applied to timestep limit MAXIMUM_TIMESTEP_BY_STELLAR_TYPE.", "rest": "(null)"}, "timestep_multiplierNOVAE": {"param_name": "timestep_multiplierNOVAE", "description": "Multiplier applied to timestep limit NOVAE.", "rest": "(null)"}, "timestep_multiplierARTIFICIAL_ACCRETION": {"param_name": "timestep_multiplierARTIFICIAL_ACCRETION", "description": "Multiplier applied to timestep limit ARTIFICIAL_ACCRETION.", "rest": "(null)"}, "timestep_multiplierSN": {"param_name": "timestep_multiplierSN", "description": "Multiplier applied to timestep limit SN.", "rest": "(null)"}, "timestep_multiplierMASS_GAIN": {"param_name": "timestep_multiplierMASS_GAIN", "description": "Multiplier applied to timestep limit MASS_GAIN.", "rest": "(null)"}, "timestep_multiplierMASS_LOSS": {"param_name": "timestep_multiplierMASS_LOSS", "description": "Multiplier applied to timestep limit MASS_LOSS.", "rest": "(null)"}, "timestep_multiplierTIDES": {"param_name": "timestep_multiplierTIDES", "description": "Multiplier applied to timestep limit TIDES.", "rest": "(null)"}, "timestep_multiplierNUCSYN_ANGELOU_LITHIUM": {"param_name": "timestep_multiplierNUCSYN_ANGELOU_LITHIUM", "description": "Multiplier applied to timestep limit NUCSYN_ANGELOU_LITHIUM.", "rest": "(null)"}, "timestep_multiplierCARBON_BURNING": {"param_name": "timestep_multiplierCARBON_BURNING", "description": "Multiplier applied to timestep limit CARBON_BURNING.", "rest": "(null)"}, "timestep_multiplierBURN_IN": {"param_name": "timestep_multiplierBURN_IN", "description": "Multiplier applied to timestep limit BURN_IN.", "rest": "(null)"}, "timestep_multiplierRADIUS_CHANGES": {"param_name": "timestep_multiplierRADIUS_CHANGES", "description": "Multiplier applied to timestep limit RADIUS_CHANGES.", "rest": "(null)"}, "timestep_multiplierMASSLESS_REMNANT": {"param_name": "timestep_multiplierMASSLESS_REMNANT", "description": "Multiplier applied to timestep limit MASSLESS_REMNANT.", "rest": "(null)"}, "timestep_multiplierORBITAL_ANGMOM": {"param_name": "timestep_multiplierORBITAL_ANGMOM", "description": "Multiplier applied to timestep limit ORBITAL_ANGMOM.", "rest": "(null)"}, "timestep_multiplierSTELLAR_ANGMOM2": {"param_name": "timestep_multiplierSTELLAR_ANGMOM2", "description": "Multiplier applied to timestep limit STELLAR_ANGMOM2.", "rest": "(null)"}, "timestep_multiplierTIDES2": {"param_name": "timestep_multiplierTIDES2", "description": "Multiplier applied to timestep limit TIDES2.", "rest": "(null)"}, "timestep_multiplierMASS_GAIN2": {"param_name": "timestep_multiplierMASS_GAIN2", "description": "Multiplier applied to timestep limit MASS_GAIN2.", "rest": "(null)"}, "timestep_multiplierMASS_LOSS2": {"param_name": "timestep_multiplierMASS_LOSS2", "description": "Multiplier applied to timestep limit MASS_LOSS2.", "rest": "(null)"}, "timestep_multiplierGRAVITATIONAL_WAVE_RADIATION": {"param_name": "timestep_multiplierGRAVITATIONAL_WAVE_RADIATION", "description": "Multiplier applied to timestep limit GRAVITATIONAL_WAVE_RADIATION.", "rest": "(null)"}, "timestep_multiplierRLOF": {"param_name": "timestep_multiplierRLOF", "description": "Multiplier applied to timestep limit RLOF.", "rest": "(null)"}, "timestep_multiplierFIXED_TIMESTEP": {"param_name": "timestep_multiplierFIXED_TIMESTEP", "description": "Multiplier applied to timestep limit FIXED_TIMESTEP.", "rest": "(null)"}, "timestep_multiplierTIME_REMAINING": {"param_name": "timestep_multiplierTIME_REMAINING", "description": "Multiplier applied to timestep limit TIME_REMAINING.", "rest": "(null)"}, "timestep_multiplierZOOMFAC": {"param_name": "timestep_multiplierZOOMFAC", "description": "Multiplier applied to timestep limit ZOOMFAC.", "rest": "(null)"}, "timestep_multiplierTHERMAL": {"param_name": "timestep_multiplierTHERMAL", "description": "Multiplier applied to timestep limit THERMAL.", "rest": "(null)"}, "timestep_multiplierNUMBER": {"param_name": "timestep_multiplierNUMBER", "description": "Multiplier applied to timestep limit NUMBER.", "rest": "(null)"}, "maximum_timestep": {"param_name": "maximum_timestep", "description": "The maximum timestep (MYr). Must not be zero.", "rest": "(null)"}, "maximum_timestep_by_stellar_type_%d": {"param_name": "maximum_timestep_by_stellar_type_%d", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_LOW_MASS_MS": {"param_name": "maximum_timestep_by_stellar_type_LOW_MASS_MS", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_MS": {"param_name": "maximum_timestep_by_stellar_type_MS", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_HG": {"param_name": "maximum_timestep_by_stellar_type_HG", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_GIANT_BRANCH": {"param_name": "maximum_timestep_by_stellar_type_GIANT_BRANCH", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_CHeB": {"param_name": "maximum_timestep_by_stellar_type_CHeB", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_EAGB": {"param_name": "maximum_timestep_by_stellar_type_EAGB", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_TPAGB": {"param_name": "maximum_timestep_by_stellar_type_TPAGB", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_HeMS": {"param_name": "maximum_timestep_by_stellar_type_HeMS", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_HeHG": {"param_name": "maximum_timestep_by_stellar_type_HeHG", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_HeGB": {"param_name": "maximum_timestep_by_stellar_type_HeGB", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_HeWD": {"param_name": "maximum_timestep_by_stellar_type_HeWD", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_COWD": {"param_name": "maximum_timestep_by_stellar_type_COWD", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_ONeWD": {"param_name": "maximum_timestep_by_stellar_type_ONeWD", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_NS": {"param_name": "maximum_timestep_by_stellar_type_NS", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_BH": {"param_name": "maximum_timestep_by_stellar_type_BH", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "maximum_timestep_by_stellar_type_MASSLESS_REMNANT": {"param_name": "maximum_timestep_by_stellar_type_MASSLESS_REMNANT", "description": "The maximum timestep by stellar type (MYr). Ignored if zero (default 0).", "rest": "(null)"}, "zoomfac_multiplier_decrease": {"param_name": "zoomfac_multiplier_decrease", "description": "When a timestep is rejected, decrease the timestep by this factor (0.5).", "rest": "(null)"}, "zoomfac_multiplier_increase": {"param_name": "zoomfac_multiplier_increase", "description": "When a timestep is rejected, zooms, then succeeds, increase the timestep by this factor (1.2).", "rest": "(null)"}, "maximum_timestep_factor": {"param_name": "maximum_timestep_factor", "description": "The maximum factor between two subsequent timesteps (1.2).", "rest": "(null)"}, "maximum_nuclear_burning_timestep": {"param_name": "maximum_nuclear_burning_timestep", "description": "The maximum timestep (MYr) in any nuclear burning phase.", "rest": "(null)"}, "nova_retention_method": {"param_name": "nova_retention_method", "description": "Algorithm used to calculate the amount of mass retained during a nova explosion. 0=use nova_retention_fraction. (other methods pending)", "rest": "(null)"}, "nova_yield_CO_algorithm": {"param_name": "nova_yield_CO_algorithm", "description": "Algorithm used to calculate the yields of COWD novae. Current options: NOVA_YIELD_CO_ALGOTHIM_JOSE_HERNANZ_1998 (0).", "rest": "(null)"}, "nova_yield_ONe_algorithm": {"param_name": "nova_yield_ONe_algorithm", "description": "Algorithm used to calculate the yields of ONeWD novae. Current options: NOVA_YIELD_ONe_ALGOTHIM_JOSE_HERNANZ_1998 (0), NOVA_YIELD_ONe_ALGORITHM_JOSE2022 (1).", "rest": "(null)"}, "MINT_metallicity": {"param_name": "MINT_metallicity", "description": "This sets the metallicity for MINT. It is ignored if set to -1.0, the default, in which case the normal metallicity parameter is used.", "rest": "(null)"}, "gaia_Teff_binwidth": {"param_name": "gaia_Teff_binwidth", "description": "log10(Effective temperature) bin width used to make Gaia-like HRDs", "rest": "(null)"}, "gaia_L_binwidth": {"param_name": "gaia_L_binwidth", "description": "log10(luminosity) bin width used to make Gaia-like HRDs", "rest": "(null)"}, "gaia_colour_transform_method": {"param_name": "gaia_colour_transform_method", "description": "Use this to select the method used to transform to Gaia colours from other colour schemes. GAIA_CONVERSION_UBVRI_UNIVARIATE_JORDI2010 = 0 Jordi et al.'s univariate UBVRI fits, GAIA_CONVERSION_UBVRI_BIVARIATE_JORDI2010 = 1 Jordi et al.'s bivariate UBVRI fits, GAIA_CONVERSION_ugriz_UNIVARIATE_JORDI2010 = 2 Jordi et al.'s univariate UBVRI fits, GAIA_CONVERSION_ugriz_BIVARIATE_JORDI2010 = 3 Jordi et al.'s univariate ugriv fits, GAIA_CONVERSION_UBVRI_UNIVARIATE_EVANS2018 = 4 Evans et al. (2018, DR2) fits, GAIA_CONVERSION_ugriz_UNIVARIATE_EVANS2018 = 5 Evans et al. (2018, DR2) fits, GAIA_CONVERSION_UBVRI_RIELLO2020 = 6 Riello et al. (2020, DR3) fits, GAIA_CONVERSION_ugriz_RIELLO2020 = 7 Riello et al. (2020, DR3) fits.", "rest": "(null)"}, "rotationally_enhanced_mass_loss": {"param_name": "rotationally_enhanced_mass_loss", "description": "Set to 1 to enable rotationally enhanced mass loss rate algorithms: 0= none, 1=formula cf. Langer models (=ROTATIONALLY_ENHANCED_MASSLOSS_LANGER_FORMULA), 2=limit accretion rate before wind loss is applied, 3 = both 1 and 2. See also rotationally_enhanced_exponent", "rest": "(null)"}, "AGB_core_algorithm": {"param_name": "AGB_core_algorithm", "description": "Algorithm to use for calculating AGB core masses. 0=Hurley et al. 2002 if no NUCSYN, Karakas 2002 if NUCSYN is defined; 1=Hurley et al. 2002 (overshooting models); 1=Karakas 2002 (non-overshooting models).", "rest": "(null)"}, "AGB_radius_algorithm": {"param_name": "AGB_radius_algorithm", "description": "Algorithm to use for calculating radii on the TPAGB.", "rest": "(null)"}, "AGB_luminosity_algorithm": {"param_name": "AGB_luminosity_algorithm", "description": "Algorithm to use for calculating luminosities on the TPAGB.", "rest": "(null)"}, "AGB_3dup_algorithm": {"param_name": "AGB_3dup_algorithm", "description": "Algorithm to use for calculating third dredge up efficiency on the TPAGB.", "rest": "(null)"}, "overspin_algorithm": {"param_name": "overspin_algorithm", "description": "Algorithm to determine what we do when a star is rotating at its breakup velocity. OVERSPIN_BSE (0) conservatively transfers the angular momentum back to the orbit. OVERSPIN_MASSLOSS uses the rotationally_enhanced_massloss parameter to lose mass which carries away the angular momentum.", "rest": "(null)"}, "rotationally_enhanced_exponent": {"param_name": "rotationally_enhanced_exponent", "description": "The exponent (power) by which rotationally enhanced mass loss is raised. Requires ROTATIONALLY_ENHANCED_MASS_LOSS. See also rotationally_enhanced_mass_loss.", "rest": "(null)"}, "batchmode": {"param_name": "batchmode", "description": "Set the batchmode control variable. Use only if you know what you are doing!", "rest": "(null)"}, "speedtests": {"param_name": "speedtests", "description": "If True, turns on speedtests during version information (off by default).", "rest": "(null)"}, "use_fixed_timestep_%d": {"param_name": "use_fixed_timestep_%d", "description": "Set to True to use fixed timestep <n>, False to turn off. Fixed timesteps are on (this is True) by default.", "rest": "(null)"}, "use_fixed_timestep_ENSEMBLE": {"param_name": "use_fixed_timestep_ENSEMBLE", "description": "Set to True to use fixed timestep ENSEMBLE, False to turn off. Fixed timesteps are on (this is True) by default.", "rest": "(null)"}, "use_fixed_timestep_TEST": {"param_name": "use_fixed_timestep_TEST", "description": "Set to True to use fixed timestep TEST, False to turn off. Fixed timesteps are on (this is True) by default.", "rest": "(null)"}, "use_fixed_timestep_NUMBER": {"param_name": "use_fixed_timestep_NUMBER", "description": "Set to True to use fixed timestep NUMBER, False to turn off. Fixed timesteps are on (this is True) by default.", "rest": "(null)"}, "task%d": {"param_name": "task%d", "description": "Control tasks to be performed by binary_c. By default, these are all TRUE. For more information see binary_c_macros.h, particularly the BINARY_C_TASK_* macros.", "rest": "(null)"}, "taskTIME_EVOLUTION": {"param_name": "taskTIME_EVOLUTION", "description": "Control tasks to be performed by binary_c. By default, these are all TRUE. For more information see binary_c_macros.h, particularly the BINARY_C_TASK_* macros.", "rest": "(null)"}, "taskCALCULATE_DERIVATIVES": {"param_name": "taskCALCULATE_DERIVATIVES", "description": "Control tasks to be performed by binary_c. By default, these are all TRUE. For more information see binary_c_macros.h, particularly the BINARY_C_TASK_* macros.", "rest": "(null)"}, "taskAPPLY_DERIVATIVES": {"param_name": "taskAPPLY_DERIVATIVES", "description": "Control tasks to be performed by binary_c. By default, these are all TRUE. For more information see binary_c_macros.h, particularly the BINARY_C_TASK_* macros.", "rest": "(null)"}, "taskCALCULATE_STELLAR_EVOLUTION": {"param_name": "taskCALCULATE_STELLAR_EVOLUTION", "description": "Control tasks to be performed by binary_c. By default, these are all TRUE. For more information see binary_c_macros.h, particularly the BINARY_C_TASK_* macros.", "rest": "(null)"}, "taskCALCULATE_BINARY_EVOLUTION": {"param_name": "taskCALCULATE_BINARY_EVOLUTION", "description": "Control tasks to be performed by binary_c. By default, these are all TRUE. For more information see binary_c_macros.h, particularly the BINARY_C_TASK_* macros.", "rest": "(null)"}, "taskNUMBER": {"param_name": "taskNUMBER", "description": "Control tasks to be performed by binary_c. By default, these are all TRUE. For more information see binary_c_macros.h, particularly the BINARY_C_TASK_* macros.", "rest": "(null)"}, "orbiting_object": {"param_name": "orbiting_object", "description": "Usage: --orbiting_object mass,spinrate,central_object,period.", "rest": "1.0"}, "orbiting_objects_log": {"param_name": "orbiting_objects_log", "description": "If True, turn on orbiting-object log.", "rest": "(null)"}, "orbiting_objects_wind_accretion_multiplier": {"param_name": "orbiting_objects_wind_accretion_multiplier", "description": "Multiplier for wind accretion on orbiting objects. Hurley et al 2002 use 1.5, which is the default.", "rest": "(null)"}, "orbiting_objects_close_pc_threshold": {"param_name": "orbiting_objects_close_pc_threshold", "description": "How close are orbiting objects allowed to be? Set this to be the absolute percentage difference minimum.", "rest": "(null)"}, "orbiting_objects_tides_multiplier": {"param_name": "orbiting_objects_tides_multiplier", "description": "Multiplier for tidal torques on orbiting objects.", "rest": "(null)"}, "evaporate_escaped_orbiting_objects": {"param_name": "evaporate_escaped_orbiting_objects", "description": "If True, evaporate orbiting objects that have escaped the system.", "rest": "(null)"}, "RLOF_transition_objects_escape": {"param_name": "RLOF_transition_objects_escape", "description": "If True, objects that escape their Roche lobe are ejected from the system, otherwise they are placed just outside the minimum stable orbit.", "rest": "(null)"}, "PN_resolve": {"param_name": "PN_resolve", "description": "If True, the timestep will be shortened to resolve better the PN phase (FALSE).", "rest": "(null)"}, "PN_resolve_minimum_luminosity": {"param_name": "PN_resolve_minimum_luminosity", "description": "The luminosity above which extra time resolution for PNe is applied (see PN_resolve).", "rest": "(null)"}, "PN_resolve_maximum_envelope_mass": {"param_name": "PN_resolve_maximum_envelope_mass", "description": "The envelope mass below which extra time resolution for PNe is applied (see PN_resolve).", "rest": "(null)"}, "PN_resolve_minimum_effective_temperature": {"param_name": "PN_resolve_minimum_effective_temperature", "description": "The minimum effective temperature above which extra time resolution for PNe is applied (see PN_resolve).", "rest": "(null)"}, "PN_fast_wind": {"param_name": "PN_fast_wind", "description": "If True, thin-envelope PNe will have fast winds (FALSE).", "rest": "(null)"}, "PN_fast_wind_dm_GB": {"param_name": "PN_fast_wind_dm_GB", "description": "The envelope mass below which fast wind used during the GB if PN_fast_wind is TRUE. (See also PN_fast_wind, PN_fast_wind_mdot_GB)", "rest": "(null)"}, "PN_fast_wind_mdot_GB": {"param_name": "PN_fast_wind_mdot_GB", "description": "The envelope mass below which fast wind used during the GB if PN_fast_wind is TRUE. (See also PN_fast_wind, PN_fast_wind_mdot_GB)", "rest": "(null)"}, "PN_fast_wind_dm_AGB": {"param_name": "PN_fast_wind_dm_AGB", "description": "The envelope mass below which fast wind used during the AGB if PN_fast_wind is TRUE. (See also PN_fast_wind, PN_fast_wind_mdot_AGB)", "rest": "(null)"}, "PN_fast_wind_mdot_AGB": {"param_name": "PN_fast_wind_mdot_AGB", "description": "The envelope mass below which fast wind used during the GB if PN_fast_wind is TRUE. (See also PN_fast_wind, PN_fast_wind_mdot_AGB)", "rest": "(null)"}, "HeWD_HeWD_ignition_mass": {"param_name": "HeWD_HeWD_ignition_mass", "description": "HeWD-HeWD mergers above this mass reignite helium. (0.3)", "rest": "(null)"}, "wind_Nieuwenhuijzen_luminosity_lower_limit": {"param_name": "wind_Nieuwenhuijzen_luminosity_lower_limit", "description": "Above this luminosity we activate the Nieuwenhuijzen and de Jager wind (4e3 Lsun).", "rest": "(null)"}, "wind_LBV_luminosity_lower_limit": {"param_name": "wind_LBV_luminosity_lower_limit", "description": "Above this luminosity we activate the LBV wind (6e5 Lsun).", "rest": "(null)"}, "colour%d": {"param_name": "colour%d", "description": "Sets colour %d (0 to NUM_ANSI_COLOURS-1) to the extended ANSI set colour you choose (1-255, 0 means ignore). The colour numbers are defined in src/logging/ansi_colours.h", "rest": "(null)"}, "apply_Darwin_Radau_correction": {"param_name": "apply_Darwin_Radau_correction", "description": "Apply Darwin-Radau correction to the moment of inertia to take rotation into account?", "rest": "(null)"}, "adjust_structure_from_mass_changes": {"param_name": "adjust_structure_from_mass_changes", "description": "If True, adjust L and R based on changes in M on the previous thermal timescale. (Currently experimental hence defaults to FALSE)", "rest": "(null)"}, "save_mass_history_n_thermal": {"param_name": "save_mass_history_n_thermal", "description": "Number of thermal timesteps of mass change history to be saved (4).", "rest": "(null)"}, "degenerate_core_merger_nucsyn": {"param_name": "degenerate_core_merger_nucsyn", "description": "If TRUE, assume that in a degnerate core merger, energy is generated from nucleosynthesis of the whole core, and that this can disrupt the core. The BSE algorithm (Hurley et al. 2002) assumes this to be TRUE, but binary_c assumes FALSE by default. (FALSE)", "rest": "(null)"}, "degenerate_core_helium_merger_ignition": {"param_name": "degenerate_core_helium_merger_ignition", "description": "If TRUE, assume that when there is a degenerate helium core merger, the star reignites helium. This is required to make R-type carbon stars. (TRUE)", "rest": "(null)"}, "degenerate_core_merger_dredgeup_fraction": {"param_name": "degenerate_core_merger_dredgeup_fraction", "description": "If non-zero, mix this fraction of the degenerate core during a merger.(0.0).", "rest": "(null)"}, "PPISN_prescription": {"param_name": "PPISN_prescription", "description": "(Pulsational) Pair-Instability Supernova prescription: handles remnant mass calculation for stars that undergo PPISN or PISN. Requires PPISN to be defined.", "rest": "Ignore"}, "PPISN_additional_massloss": {"param_name": "PPISN_additional_massloss", "description": "(Pulsational) Pair-Instability Supernova additional mass loss on top of that given by the chosen prescription. Requires PPISN to be defined.", "rest": "Ignore"}, "PPISN_core_mass_range_shift": {"param_name": "PPISN_core_mass_range_shift", "description": "(Pulsational) Pair-Instability Supernova CO core mass range shift: Mass by which we shift the range of CO core mass that undergoes PPISN. This is taken into account in the fit that calculates mass removal. Negative shifts the range to lower masses, positive to higher masses. Requires PPISN to be defined.", "rest": "Ignore"}, "PPISN_massloss_multiplier": {"param_name": "PPISN_massloss_multiplier", "description": "(Pulsational) Pair-Instability Supernova CO mass loss multiplier. Currently only works with the new prescription. Does not change additional mass loss. Requires PPISN to be defined.", "rest": "Ignore"}, "fixed_beta_mass_transfer_efficiency": {"param_name": "fixed_beta_mass_transfer_efficiency", "description": "Parameter to fix mass transfer efficiency. Choosing a value between 0 and 1 enables this functionality and disables the rate limiters accretion_limit_thermal_multiplier and accretion_limit_dynamical_multiplier, and sets the accretion efficiency to the value provided or that of the Eddington accretion limit (whichever has the most excess). Default value is FIXED_BETA_MASS_TRANSFER_EFFICIENCY_DISABLED == -1.0, which disables this functionality.", "rest": "Ignore"}, "circumstellar_disk": {"param_name": "circumstellar_disk", "description": "Flag to activate circumstellar disk (mass loss) physics.", "rest": "Ignore"}, "circumstellar_disk_outer_edge_location_prescription": {"param_name": "circumstellar_disk_outer_edge_location_prescription", "description": "Prescription to select the disc outer edge location. TODO: implement prescriptions", "rest": "Ignore"}, "circumstellar_disk_L2_mass_loss_prescription": {"param_name": "circumstellar_disk_L2_mass_loss_prescription", "description": "Prescription that determines the rate of mass flowing out of the L2 point due to disk mass loss. TODO: implement prescriptions", "rest": "Ignore"}, "circumstellar_disk_L2_mass_loss_multiplier": {"param_name": "circumstellar_disk_L2_mass_loss_multiplier", "description": "Multiplier for the L2 outflow rate of circumstellar disks. The outflow rate will be limited based on mass and angular momentum conservation on default  (see parameters 'circumstellar_disk_apply_mass_conservation_check' and 'circumstellar_disk_apply_angular_momentum_conservation_check').", "rest": "Ignore"}, "circumstellar_disk_isotropic_mass_loss_prescription": {"param_name": "circumstellar_disk_isotropic_mass_loss_prescription", "description": "Prescription that determines the fraction of transferred mass due to disk mass loss isotropically. TODO: implement prescriptions", "rest": "Ignore"}, "circumstellar_disk_isotropic_mass_loss_multiplier": {"param_name": "circumstellar_disk_isotropic_mass_loss_multiplier", "description": "Multiplier for the isotropic outflow rate of circumstellar disks. The outflow rate will be limited based on mass and angular momentum conservation on default (see parameters 'circumstellar_disk_apply_mass_conservation_check' and 'circumstellar_disk_apply_angular_momentum_conservation_check').", "rest": "Ignore"}, "circumstellar_disk_apply_mass_conservation_check": {"param_name": "circumstellar_disk_apply_mass_conservation_check", "description": "Flag to control the mass conservation check and limiter. The limiter will limit the suggested mass loss rate based on the available mass transfer rate. default = 1. 0 = False, 1 = True.", "rest": "Ignore"}, "circumstellar_disk_apply_angular_momentum_conservation_check": {"param_name": "circumstellar_disk_apply_angular_momentum_conservation_check", "description": "Flag to control the angular_momentum conservation check and limiter. The limiter will limit the suggested mass loss rate based on the available angular momentum transfer rate. default = 1. 0 = False, 1 = True.", "rest": "Ignore"}, "circumstellar_disk_apply_derivative_updates": {"param_name": "circumstellar_disk_apply_derivative_updates", "description": "Flag to control whether we apply the derivative updates for the changes introduced by the disc ML.", "rest": "Ignore"}, "circumstellar_disk_account_for_radial_expansion_of_strongly_rotating_accretor": {"param_name": "circumstellar_disk_account_for_radial_expansion_of_strongly_rotating_accretor", "description": "Flag to control whether radial expansion of the accretor (when rotating very rapidly) is taken into account in the direct impact calculations and in the accretion radius calculations.", "rest": "Ignore"}, "RLOF_enable_stream_integration_project": {"param_name": "RLOF_enable_stream_integration_project", "description": "Flag to use the custom mass stream integration project functions. This includes using an updated r_min and r_circ routine, self-accretion onto the donor and more TODO: expand which things are included in this. 0 = Disabled. 1 = Enabled.", "rest": "Ignore"}, "RLOF_rmin_prescription": {"param_name": "RLOF_rmin_prescription", "description": "Radius of closest approach (rmin) prescription. RLOF_RMIN_PRESCRIPTION_ULRICH_BURGER: standard ulrich-burger implementation. RLOF_RMIN_PRESCRIPTION_ULRICH_BURGER_SCALED: ulrich-burger rmin scaled by the fraction of synchronicity of donor f = w_don/w_orb, based on angular momentum considerations. RLOF_RMIN_PRESCRIPTION_HENDRIKS2022_INTERPOLATION: rmin calculated through an interpolation table that takes q_acc = m_acc/m_don and f = w_don/w_orb", "rest": "Ignore"}, "RLOF_rcirc_prescription": {"param_name": "RLOF_rcirc_prescription", "description": "Circularisation radius (rcirc) prescription. RLOF_RCIRC_PRESCRIPTION_ULRICH_BURGER: standard ulrich-burger implementation. RLOF_RCIRC_PRESCRIPTION_HENDRIKS2022_INTERPOLATION: rcirc calculated through an interpolation table that takes q_acc = m_acc/m_don and f = w_don/w_orb", "rest": "Ignore"}, "RLOF_lagrange_point_prescription": {"param_name": "RLOF_lagrange_point_prescription", "description": "Lagrange point calculation prescription. The choice here affects the calculation of the lagrange point locations, as well as the roche lobe radius calculations.  RLOF_LAGRANGE_POINT_PRESCRIPTION_BINARY_C: standard lagrange point calculation based on circular orbits and co-rotating donors. RLOF_LAGRANGE_POINT_PRESCRIPTION_SEPINSKY2007: more detailed calculation for the lagrange points that takes into account eccentric orbits, and asynchronously rotating donors, based on Sepinsky 2007, and based on the first-approximation method to calculate the potential.", "rest": "Ignore"}, "CHE_enabled": {"param_name": "CHE_enabled", "description": "Global switch for enabling the CHE functionality. disabled = 0 (default), enabled = 1", "rest": "Ignore"}, "CHE_determination_prescription": {"param_name": "CHE_determination_prescription", "description": "Prescription to determine whether a star will start to evolve chemically homogeneously (CHE).", "rest": "Ignore"}, "CHE_enable_ensemble_logging": {"param_name": "CHE_enable_ensemble_logging", "description": "Flag to enable CHE ensemble output. This probably should be moved to a proper ensemble filter but for now i'm putting this here", "rest": "Ignore"}, "custom_timeout_time": {"param_name": "custom_timeout_time", "description": "Custom timeout time. Requires compilation with DAVID_CUSTOM_TIMEOUT", "rest": "(null)"}, "use_LWN_fallback": {"param_name": "use_LWN_fallback", "description": "Flag whether to use the Nazehdin-Lovegrove-Woosley hydrogen envelope ejection at failed supernova.", "rest": "Ignore"}, "prevent_LWN_kick": {"param_name": "prevent_LWN_kick", "description": "Flag whether to prevent a blaauw-type kick induced by LWN mass loss. See use_LWN_fallback", "rest": "Ignore"}}}, "binary": {"section_name": "binary", "parameters": {"separation": {"param_name": "separation", "description": "Set the orbital separation (actually the semi-major axis) of the binary (internal index 0, stellar indices 0 and 1) in solar radii. Note that if the orbital period is given, it is used to calculate the separation and the value you set with this argument is ignored. So if you want to set the separation instead, either do not set the orbital period or set the orbital period to zero (0.0).", "rest": "(null)"}, "separation_triple": {"param_name": "separation_triple", "description": "Set the orbital separation (actually the semi-major axis) of the triple (internal index 1) in solar radii. Note that if the orbital period is given, it is used to calculate the separation. So if you want to set the separation instead, either do not set the orbital period or set the orbital period to zero (0.0).", "rest": "(null)"}, "separation_quadruple": {"param_name": "separation_quadruple", "description": "Set the orbital separation (actually the semi-major axis) of the quadruple (internal index 2) in solar radii. Note that if the orbital period is given, it is used to calculate the separation. So if you want to set the separation instead, either do not set the orbital period or set the orbital period to zero (0.0).", "rest": "(null)"}, "orbital_period": {"param_name": "orbital_period", "description": "Set the initial orbital period of the binary, stars 1 and 2 (internal indices 0 and 1) in days. See also separation.", "rest": "(null)"}, "orbital_period_triple": {"param_name": "orbital_period_triple", "description": "Set the initial orbital period of the triple in days. See also separation.", "rest": "(null)"}, "orbital_period_quadruple": {"param_name": "orbital_period_quadruple", "description": "Set the orbital period of the outer binary in a quadrulple (stars 3 and 4, internal indices 2 and 3) in days. See also separation.", "rest": "(null)"}, "eccentricity": {"param_name": "eccentricity", "description": "Set the initial eccentricity of the binary orbit (stars 1 and 2, internal indices 0 and 1).", "rest": "(null)"}, "eccentricity_triple": {"param_name": "eccentricity_triple", "description": "Set the initial eccentricity of the triple orbit.", "rest": "(null)"}, "eccentricity_quadruple": {"param_name": "eccentricity_quadruple", "description": "Set the initial eccentricity of the outer binary of a quadruple (stars 3 and 4, internal indices 2 and 3).", "rest": "(null)"}, "incliniation": {"param_name": "incliniation", "description": "Set the initial orbital_inclination of the binary relative to zero.", "rest": "(null)"}, "incliniation_triple": {"param_name": "incliniation_triple", "description": "Set the initial orbital_inclination of the triple orbit relative to zero.", "rest": "(null)"}, "incliniation_quadruple": {"param_name": "incliniation_quadruple", "description": "Set the initial orbital_inclinationy of the quadruple orbit relative to zero.", "rest": "(null)"}, "orbital_phase": {"param_name": "orbital_phase", "description": "Set the initial orbital phase of the binary orbit.", "rest": "(null)"}, "orbital_phase_triple": {"param_name": "orbital_phase_triple", "description": "Set the initial orbital phase of the triple orbit.", "rest": "(null)"}, "orbital_phase_quadruple": {"param_name": "orbital_phase_quadruple", "description": "Set the initial orbital phase of the quadruple orbit.", "rest": "(null)"}, "argument_of_periastron": {"param_name": "argument_of_periastron", "description": "Set the initial argument of periastron of the binary orbit.", "rest": "(null)"}, "argument_of_periastron_triple": {"param_name": "argument_of_periastron_triple", "description": "Set the initial argument of periastron of the triple orbit.", "rest": "(null)"}, "argument_of_periastron_quadruple": {"param_name": "argument_of_periastron_quadruple", "description": "Set the initial argument of periastron of the quadruple orbit.", "rest": "(null)"}, "disc_timestep_factor": {"param_name": "disc_timestep_factor", "description": "Factor that multiplies the natural timestep of a disc.", "rest": "(null)"}, "white_dwarf_cooling_model": {"param_name": "white_dwarf_cooling_model", "description": "White dwarf cooling model, relates age to luminosity. WHITE_DWARF_COOLING_MESTEL = 0 is Mestel's model, WHITE_DWARF_COOLING_MESTEL_MODIFIED = 1 is Hurley's modified Mestel model, WHITE_DWARF_COOLING_CARRASCO2014 = 2 is based on Carrasco (2014) tables.  ", "rest": "(null)"}, "white_dwarf_radius_model": {"param_name": "white_dwarf_radius_model", "description": "White dwarf radius model, radius to mass (and perhaps age). WHITE_DWARF_RADIUS_NAUENBERG1972 = 0 Nauenberg (1972), WHITE_DWARF_RADIUS_MU = 1 mu-dependent variant, WHITE_DWARF_RADIUS_CARRASCO2014 = 2 is based on Carrasco (2014) tables.", "rest": "(null)"}, "cbdisc_mass_loss_inner_viscous_accretion_method": {"param_name": "cbdisc_mass_loss_inner_viscous_accretion_method", "description": "Chooses where the mass that is accreted from the inner edge of a circumbinary disc goes, i.e. to which star. 0 = Young and Clarke 2015, 1 = Gerosa et al 2015, 2 = 50:50 (i.e. not dependence on mass).", "rest": "(null)"}, "cbdisc_inner_edge_stripping": {"param_name": "cbdisc_inner_edge_stripping", "description": "If True, allow inner edge mass stripping.", "rest": "(null)"}, "cbdisc_end_evolution_after_disc": {"param_name": "cbdisc_end_evolution_after_disc", "description": "If True, stop evolution when a disc evaporates.", "rest": "(null)"}, "cbdisc_no_wind_if_cbdisc": {"param_name": "cbdisc_no_wind_if_cbdisc", "description": "If True, disable stellar winds when there is a circumbinary disc.", "rest": "(null)"}, "cbdisc_outer_edge_stripping": {"param_name": "cbdisc_outer_edge_stripping", "description": "If True, allow outer edge mass stripping.", "rest": "(null)"}, "disc_n_monte_carlo_guesses": {"param_name": "disc_n_monte_carlo_guesses", "description": "Number of monte carlo guesses to try in the disc solver if the normal list of guesses fails (0).", "rest": "(null)"}, "disc_log": {"param_name": "disc_log", "description": "If 1, turn on the disc log. Requires DISC_LOG to be defined on build.", "rest": "(null)"}, "disc_log2d": {"param_name": "disc_log2d", "description": "If 1, turn on the 2d disc log. Requires DISC_LOG to be defined on build.", "rest": "(null)"}, "disc_log_dt": {"param_name": "disc_log_dt", "description": "If non-zero, only allows disc log output every disc_log_dt Myr.", "rest": "(null)"}, "disc_log_directory": {"param_name": "disc_log_directory", "description": "Directory into which disc logging is sent (must exist!).", "rest": "/tmp/"}, "post_ce_adaptive_menv": {"param_name": "post_ce_adaptive_menv", "description": "If TRUE, and if post_ce_objects_have_envelopes is TRUE, then the envelope mass of a post-CE star is such that it sits just inside its Roche lobe. If FALSE then a fixed (thin) envelope mass is applied that depends on the stellar type (see macros POST_CE_ENVELOPE_DM_GB, POST_CE_ENVELOPE_DM_EAGB and POST_CE_ENVELOPE_DM_TPAGB).", "rest": "(null)"}, "post_ce_objects_have_envelopes": {"param_name": "post_ce_objects_have_envelopes", "description": "If TRUE then post-common-envelope objects have thin envelopes. You need this if you are to have post-CE post-AGB stars. Note that this *may* be unstable, i.e. you may end up having many CEEs. The mass in the envelope is controlled by post_ce_adaptive_menv. TRUE by default.", "rest": "(null)"}, "PN_comenv_transition_time": {"param_name": "PN_comenv_transition_time", "description": "post-common envelope transition time in years (1e2).  This is the time taken to move from CEE ejection to Teff > 30e4 K. Hall et al. (2013) suggest ~100 years.", "rest": "(null)"}, "minimum_time_between_PNe": {"param_name": "minimum_time_between_PNe", "description": "The minimum time (Myr) between planetary nebula detections. This prevents multiple, fast common envelopes triggering two PNe (0.1).", "rest": "(null)"}, "PN_Hall_fading_time_algorithm": {"param_name": "PN_Hall_fading_time_algorithm", "description": "In stars with low mass (<0.45Msun) cores, you can choose to set the PN fading time to either the minimum (PN_HALL_FADING_TIME_ALGORITHM_MINIMUM) or maximum (PN_HALL_FADING_TIME_ALGORITHM_MAXIMUM) as shown in Fig. 6 of Hall et al. (2013).", "rest": "(null)"}, "PPN_envelope_mass": {"param_name": "PPN_envelope_mass", "description": "Desired pre-planetary nebula (post-AGB) envelope mass.", "rest": "(null)"}, "cbdisc_eccentricity_pumping_method": {"param_name": "cbdisc_eccentricity_pumping_method", "description": "Select from various eccentricity-pumping methods when there is a circumbinary disc. Requires DISCS. 0 = off.", "rest": "(null)"}, "cbdisc_viscous_photoevaporative_coupling": {"param_name": "cbdisc_viscous_photoevaporative_coupling", "description": "Set to 1 to turn on viscous-photoevaporative coupling in circumbinary discs. Requires DISCS. 0 = CBDISC_VISCOUS_PHOTOEVAPORATIVE_COUPLING_NONE = off, 1 = CBDISC_VISCOUS_PHOTOEVAPORATIVE_COUPLING_INSTANT instant, 2 = CBDISC_VISCOUS_PHOTOEVAPORATIVE_COUPLING_VISCOUS slow, viscous wind.", "rest": "(null)"}, "cbdisc_inner_edge_stripping_timescale": {"param_name": "cbdisc_inner_edge_stripping_timescale", "description": "Defines the timescale for mass loss from by inner edge stripping. 0 = instant, 1 = very long, 2 = viscous at Revap_in, 3 = orbital at Revap_in.", "rest": "(null)"}, "cbdisc_outer_edge_stripping_timescale": {"param_name": "cbdisc_outer_edge_stripping_timescale", "description": "Defines the timescale for mass loss from by outer edge stripping. 0 = instant, 1 = very long, 2 = viscous at Revap_in, 3 = orbital at Revap_out.", "rest": "(null)"}, "cbdisc_viscous_L2_coupling": {"param_name": "cbdisc_viscous_L2_coupling", "description": "Set to 1 to turn on viscous-L2-loss coupling in circumbinary discs. Requires DISCS. 0 = off.", "rest": "(null)"}, "gravitational_radiation_model": {"param_name": "gravitational_radiation_model", "description": "Model for gravitational radiation from the system. 0=Hurley et al 2002 (Landau and Lifshitz 1951). 1 = as 0 but only when there is no RLOF. 2 = none.", "rest": "(null)"}, "nova_irradiation_multiplier": {"param_name": "nova_irradiation_multiplier", "description": "Multiplier for nova-radiative induced mass loss. (Shara+1986)", "rest": "(null)"}, "gravitational_radiation_modulator_J": {"param_name": "gravitational_radiation_modulator_J", "description": "Modulator for gravitational wave radiation angular momentum loss rate (1.0).", "rest": "(null)"}, "gravitational_radiation_modulator_e": {"param_name": "gravitational_radiation_modulator_e", "description": "Modulator for gravitational wave radiation eccentricity pumping rate (1.0).", "rest": "(null)"}, "nova_faml_multiplier": {"param_name": "nova_faml_multiplier", "description": "Nova friction-induced angular momentum loss multiplier. (Shara+1986)", "rest": "(null)"}, "RLOF_angular_momentum_transfer_model": {"param_name": "RLOF_angular_momentum_transfer_model", "description": "Choose angular momentum transfer model in RLOF. 0=BSE (with discs), 1=conservative", "rest": "(null)"}, "post_SN_orbit_method": {"param_name": "post_SN_orbit_method", "description": "Method by which the post-SN orbit is calculated. 0=BSE, 1=Tauris&Taken 1998.", "rest": "(null)"}, "multiplicity": {"param_name": "multiplicity", "description": "Multiplicity: 1=single star, 2=binary, 3=triple, 4=quadruple.", "rest": "(null)"}, "accretion_limit_eddington_steady_multiplier": {"param_name": "accretion_limit_eddington_steady_multiplier", "description": "Steady accretion is limited by the Eddington instability, with limiting rate given by the accretion_limit_eddington_steady_multiplier * the normal (spherically symmetric) Eddington rate. This is known in the trade as the Eddington factor, and anything greater than 1.0 potentially gives you super-Eddington accretion.", "rest": "(null)"}, "accretion_limit_eddington_LMMS_multiplier": {"param_name": "accretion_limit_eddington_LMMS_multiplier", "description": "Accretion from a low-mass, convective, main_sequence star is limited by the Eddington instability, with limiting rate given by the accretion_limit_eddington_LMMS_multiplier * the normal (spherically symmetric) Eddington rate. This is known in the trade as the Eddington factor, and anything greater than 1.0 potentially gives you super-Eddington accretion.", "rest": "(null)"}, "accretion_limit_eddington_WD_to_remnant_multiplier": {"param_name": "accretion_limit_eddington_WD_to_remnant_multiplier", "description": "Accretion from a WD onto a remnant star (e.g. another white dwarf, neutron star or black hole) is limited by the Eddington instability, with limiting rate given by the accretion_limit_eddington_WD_to_remnant_multiplier * the normal (spherically symmetric) Eddington rate. This is known in the trade as the Eddington factor, and anything greater than 1.0 potentially gives you super-Eddington accretion.", "rest": "(null)"}, "accretion_limit_thermal_multiplier": {"param_name": "accretion_limit_thermal_multiplier", "description": "Mass transfer onto a MS, HG or CHeB star is limited by the accretor's thermal rate times this multiplier.", "rest": "(null)"}, "accretion_limit_dynamical_multiplier": {"param_name": "accretion_limit_dynamical_multiplier", "description": "Mass transfer is limited by the accretor's dynamical rate times this multiplier.", "rest": "(null)"}, "donor_limit_envelope_multiplier": {"param_name": "donor_limit_envelope_multiplier", "description": "Mass transfer by RLOF is limited by this fraction of the donor's envelope mass per timestep", "rest": "(null)"}, "donor_limit_thermal_multiplier": {"param_name": "donor_limit_thermal_multiplier", "description": "Mass transfer by RLOF is limited by the accretor's thermal rate times this multiplier.", "rest": "(null)"}, "donor_limit_dynamical_multiplier": {"param_name": "donor_limit_dynamical_multiplier", "description": "Mass transfer by RLOF is limited by the donor's dynamical rate times this multiplier.", "rest": "(null)"}, "Bondi_Hoyle_accretion_factor": {"param_name": "Bondi_Hoyle_accretion_factor", "description": "Wind accretion rate, as calculated by the Bondi-Hoyle-Littleton formula, multiplcation factor. Hurley et al 2002 use 1.5, which is the default.", "rest": "(null)"}, "tidal_strength_factor": {"param_name": "tidal_strength_factor", "description": "A modulator for the tidal strength. If this factor > 1 then tides are stronger, i.e. tidal timescales are reduced.", "rest": "(null)"}, "tides_variable_filename": {"param_name": "tides_variable_filename", "description": "Filename pointing to a table of data to be interpolated to compute the tidal strength multiplier.", "rest": "(null)"}, "hachisu_qcrit": {"param_name": "hachisu_qcrit", "description": "Critical q=Maccretor/Mdonor above which Hachisu's disk wind turns on.", "rest": "(null)"}, "hachisu_disk_wind": {"param_name": "hachisu_disk_wind", "description": "Set to True to turn on Hachisu's disk wind when material accretes too fast onto a white dwarf. This helps to make more SNeIa. See also hachisu_qcrit.", "rest": "(null)"}, "mass_accretion_for_eld": {"param_name": "mass_accretion_for_eld", "description": "The mass that must be accreted onto a COWD for it to ignite as an edge-lit detonation SNIa.", "rest": "(null)"}, "WDWD_merger_algorithm": {"param_name": "WDWD_merger_algorithm", "description": "Algorithm to be used when merging two white dwarfs. 0 = Hurley et al. (2002), 1 = Perets+ (2019), 2 = Chen+ (2016, todo) ", "rest": "(null)"}, "eta_violent_WDWD_merger": {"param_name": "eta_violent_WDWD_merger", "description": "energy factor used to calculate q_crit for WDWD mergers that are \"violent\". Default = 0.75 (Ruiter 2013).", "rest": "(null)"}, "COWD_COWD_explode_above_mass": {"param_name": "COWD_COWD_explode_above_mass", "description": "COWD-COWD mergers above this mass trigger a SNIa.", "rest": "(null)"}, "HeWD_COWD_explode_above_mass": {"param_name": "HeWD_COWD_explode_above_mass", "description": "HeWD-COWD mergers above this mass trigger a SNIa.", "rest": "(null)"}, "COWD_to_ONeWD_accretion_rate": {"param_name": "COWD_to_ONeWD_accretion_rate", "description": "Accretion rate above which COWDs are converted to ONeWDs, in Msun/yr. A typical value is 2.05e-6 (Wang et al. 2017).  Ignored if 0 (default 0).", "rest": "(null)"}, "type_Ia_MCh_supernova_algorithm": {"param_name": "type_Ia_MCh_supernova_algorithm", "description": "Algorithm to be used when calculating type Ia yields from Chandrasekhar-mass exploders. 0 = DD7 (Iwamoto 1999), 1 = Seitenzahl 2013 3D hydro yields (you must also set Seitenzahl2013_model) ", "rest": "(null)"}, "core_collapse_supernova_algorithm": {"param_name": "core_collapse_supernova_algorithm", "description": "Algorithm to be used to determine core-collapse supernova yields.", "rest": "(null)"}, "electron_capture_supernova_algorithm": {"param_name": "electron_capture_supernova_algorithm", "description": "Algorithm to be used to determine electron-capture supernova yields.", "rest": "(null)"}, "core_collapse_rprocess_algorithm": {"param_name": "core_collapse_rprocess_algorithm", "description": "Algorithm to be used to determine core-collapse r-process yields. (Default 0 = NUCSYN_CCSNE_RPROCESS_SIMMERER2004.", "rest": "(null)"}, "core_collapse_rprocess_mass": {"param_name": "core_collapse_rprocess_mass", "description": "Mass of r-process material to be associated with a core-collapse supernova.", "rest": "(null)"}, "Seitenzahl2013_model": {"param_name": "Seitenzahl2013_model", "description": "Which of Seitenzahl et al. 2013's models to use? One of N1,N3,N5,N10,N20,N40,N100L,N100,N100H,N150,N200,N300C,N1600,N1600C,N100_Z0.5,N100_Z0.1,N100_Z0.01 (defaults to N100).", "rest": "N1"}, "type_Ia_sub_MCh_supernova_algorithm": {"param_name": "type_Ia_sub_MCh_supernova_algorithm", "description": "Algorithm to be used when calculating type Ia yields from sub-Chandrasekhar-mass exploders. (Currently unused.)", "rest": "(null)"}, "max_HeWD_mass": {"param_name": "max_HeWD_mass", "description": "The maximum mass a HeWD can have before it ignites helium (0.7).", "rest": "(null)"}, "merger_mass_loss_fraction": {"param_name": "merger_mass_loss_fraction", "description": "Fraction of the total mass which is lost when stars merge. Note: if merger_mass_loss_fraction_by_stellar_type_<n> is set, where <n> is the stellar type, it is used in place of the value of merger_mass_loss_fraction. Can be a positive number, zero, or an algorithm from: MERGER_MASS_LOSS_FRACTION_GLEBBEEK_2013.", "rest": "(null)"}, "merger_mass_loss_fraction_nondegenerate": {"param_name": "merger_mass_loss_fraction_nondegenerate", "description": "Equivalent to setting the merger_mass_loss_fraction_by_stellar_type for all nuclear-burning, non-degenerate stellar types (including low-mass main-sequence stars). Note: you should not combine this with attempts to set the mass loss fractions individually.", "rest": "(null)"}, "merger_mass_loss_fraction_degenerate": {"param_name": "merger_mass_loss_fraction_degenerate", "description": "Equivalent to setting the merger_mass_loss_fraction_by_stellar_type for all (compact) degenerate (i.e. WD, NS) stellar types. Note: you should not combine this with attempts to set the mass loss fractions individually.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_%d": {"param_name": "merger_mass_loss_fraction_by_stellar_type_%d", "description": "Fraction of the total mass which is lost when stars merge to stellar type <n>.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_LOW_MASS_MS": {"param_name": "merger_mass_loss_fraction_by_stellar_type_LOW_MASS_MS", "description": "Fraction of the total mass which is lost when stars merge to stellar type LOW_MASS_MS.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_MS": {"param_name": "merger_mass_loss_fraction_by_stellar_type_MS", "description": "Fraction of the total mass which is lost when stars merge to stellar type MS.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_HG": {"param_name": "merger_mass_loss_fraction_by_stellar_type_HG", "description": "Fraction of the total mass which is lost when stars merge to stellar type HG.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_GIANT_BRANCH": {"param_name": "merger_mass_loss_fraction_by_stellar_type_GIANT_BRANCH", "description": "Fraction of the total mass which is lost when stars merge to stellar type GIANT_BRANCH.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_CHeB": {"param_name": "merger_mass_loss_fraction_by_stellar_type_CHeB", "description": "Fraction of the total mass which is lost when stars merge to stellar type CHeB.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_EAGB": {"param_name": "merger_mass_loss_fraction_by_stellar_type_EAGB", "description": "Fraction of the total mass which is lost when stars merge to stellar type EAGB.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_TPAGB": {"param_name": "merger_mass_loss_fraction_by_stellar_type_TPAGB", "description": "Fraction of the total mass which is lost when stars merge to stellar type TPAGB.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_HeMS": {"param_name": "merger_mass_loss_fraction_by_stellar_type_HeMS", "description": "Fraction of the total mass which is lost when stars merge to stellar type HeMS.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_HeHG": {"param_name": "merger_mass_loss_fraction_by_stellar_type_HeHG", "description": "Fraction of the total mass which is lost when stars merge to stellar type HeHG.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_HeGB": {"param_name": "merger_mass_loss_fraction_by_stellar_type_HeGB", "description": "Fraction of the total mass which is lost when stars merge to stellar type HeGB.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_HeWD": {"param_name": "merger_mass_loss_fraction_by_stellar_type_HeWD", "description": "Fraction of the total mass which is lost when stars merge to stellar type HeWD.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_COWD": {"param_name": "merger_mass_loss_fraction_by_stellar_type_COWD", "description": "Fraction of the total mass which is lost when stars merge to stellar type COWD.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_ONeWD": {"param_name": "merger_mass_loss_fraction_by_stellar_type_ONeWD", "description": "Fraction of the total mass which is lost when stars merge to stellar type ONeWD.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_NS": {"param_name": "merger_mass_loss_fraction_by_stellar_type_NS", "description": "Fraction of the total mass which is lost when stars merge to stellar type NS.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_BH": {"param_name": "merger_mass_loss_fraction_by_stellar_type_BH", "description": "Fraction of the total mass which is lost when stars merge to stellar type BH.", "rest": "(null)"}, "merger_mass_loss_fraction_by_stellar_type_MASSLESS_REMNANT": {"param_name": "merger_mass_loss_fraction_by_stellar_type_MASSLESS_REMNANT", "description": "Fraction of the total mass which is lost when stars merge to stellar type MASSLESS_REMNANT.", "rest": "(null)"}, "transient_method": {"param_name": "transient_method", "description": "Choose the method used to model transients. Options: TRANSIENT_METHOD_NONE, TRANSIENT_METHOD_IVANOVA2013", "rest": "(null)"}, "merger_angular_momentum_factor": {"param_name": "merger_angular_momentum_factor", "description": "When two stars merge the resulting single star retains a fraction of the total system angular momentum (or the critical spin angular momentum, if it is smaller) multiplied by this factor.", "rest": "(null)"}, "wind_angular_momentum_loss": {"param_name": "wind_angular_momentum_loss", "description": "Prescription for losing angular momentum in a stellar wind. 0=Hurley et al 2002 ('Tout') prescription, 1=lw i.e. a factor multiplying the specific orbital angular momentum, 2=lw hybrid for fast winds. Set wind_djorb_fac to the desired factor..", "rest": "(null)"}, "wind_djorb_fac": {"param_name": "wind_djorb_fac", "description": "Factor multiplying angular momentum loss in a stellar wind when wind_angular_momentum_loss=0 (the Tout/Hurley et al 2002 prescription). See wind_angular_momentum_loss.", "rest": "(null)"}, "lw": {"param_name": "lw", "description": "Factor multiplying angular momentum loss in a stellar wind when wind_angular_momentum_loss=1,2 (the 'lw' prescription). See wind_angular_momentum_loss.", "rest": "(null)"}, "VW93_EAGB_wind_speed": {"param_name": "VW93_EAGB_wind_speed", "description": "Activate this to use Vassiliadis and Wood (1993) wind speed during the EAGB.", "rest": "(null)"}, "VW93_TPAGB_wind_speed": {"param_name": "VW93_TPAGB_wind_speed", "description": "Activate this to use Vassiliadis and Wood (1993) wind speed during the EAGB.", "rest": "(null)"}, "use_periastron_Roche_radius": {"param_name": "use_periastron_Roche_radius", "description": "Set this to True to use the Roche lobe radius at periastron, rather than (the default to) assume a circular orbit. This will be useful one day when we treat RLOF in eccentric orbits properly, hopefully.", "rest": "(null)"}, "qcrit_nuclear_burning": {"param_name": "qcrit_nuclear_burning", "description": "Set qcrit, the critical mass ratio for stable mass transfer, for all nuclear-burning donors irrespective of the accretor stellar type.", "rest": "(null)"}, "qcrit_WD": {"param_name": "qcrit_WD", "description": "Set qcrit, the critical mass ratio for stable mass transfer, for all WD donors irrespective of the accretor stellar type.", "rest": "(null)"}, "qcrit_all": {"param_name": "qcrit_all", "description": "Set qcrit, the critical mass ratio for stable mass transfer, for all donors irrespective of donor or accretor stellar type.", "rest": "(null)"}, "qcrit_LMMS": {"param_name": "qcrit_LMMS", "description": "Apply critical q=Mdonor/Maccretor value for low-mass main sequence stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_MS": {"param_name": "qcrit_MS", "description": "Apply critical q=Mdonor/Maccretor value for (non-low mass) main sequence stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_HG": {"param_name": "qcrit_HG", "description": "Apply critical q=Mdonor/Maccretor value for Hertzsprung gap stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_GB": {"param_name": "qcrit_GB", "description": "Apply critical q=Mdonor/Maccretor value for first red giant branch stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_CHeB": {"param_name": "qcrit_CHeB", "description": "Apply critical q=Mdonor/Maccretor value for core helium burning stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_EAGB": {"param_name": "qcrit_EAGB", "description": "Apply critical q=Mdonor/Maccretor value for early-AGB stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_TPAGB": {"param_name": "qcrit_TPAGB", "description": "Apply critical q=Mdonor/Maccretor value for TP-AGB stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_HeMS": {"param_name": "qcrit_HeMS", "description": "Apply critical q=Mdonor/Maccretor value for helium main sequence stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_HeHG": {"param_name": "qcrit_HeHG", "description": "Apply critical q=Mdonor/Maccretor value for helium Hertzsprung gap stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_HeGB": {"param_name": "qcrit_HeGB", "description": "Apply critical q=Mdonor/Maccretor value for helium red giant stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_HeWD": {"param_name": "qcrit_HeWD", "description": "Apply critical q=Mdonor/Maccretor value for helium white dwarf stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_COWD": {"param_name": "qcrit_COWD", "description": "Apply critical q=Mdonor/Maccretor value for carbon-oxygen white dwarf stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_ONeWD": {"param_name": "qcrit_ONeWD", "description": "Apply critical q=Mdonor/Maccretor value for oxygen-neon white dwarf stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_NS": {"param_name": "qcrit_NS", "description": "Apply critical q=Mdonor/Maccretor value for neutron stars to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_BH": {"param_name": "qcrit_BH", "description": "Apply critical q=Mdonor/Maccretor value for black holes to determine the stability of Roche-lobe overflow for non-degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_LMMS": {"param_name": "qcrit_degenerate_LMMS", "description": "Apply critical q=Mdonor/Maccretor value for (low mass) main sequence stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_MS": {"param_name": "qcrit_degenerate_MS", "description": "Apply critical q=Mdonor/Maccretor value for (non-low mass) main sequence stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_HG": {"param_name": "qcrit_degenerate_HG", "description": "Apply critical q=Mdonor/Maccretor value for Hertzsprung gap stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_GB": {"param_name": "qcrit_degenerate_GB", "description": "Apply critical q=Mdonor/Maccretor value for first red giant branch stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_CHeB": {"param_name": "qcrit_degenerate_CHeB", "description": "Apply critical q=Mdonor/Maccretor value for core helium burning stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_EAGB": {"param_name": "qcrit_degenerate_EAGB", "description": "Apply critical q=Mdonor/Maccretor value for early-AGB stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_TPAGB": {"param_name": "qcrit_degenerate_TPAGB", "description": "Apply critical q=Mdonor/Maccretor value for TP-AGB stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_HeMS": {"param_name": "qcrit_degenerate_HeMS", "description": "Apply critical q=Mdonor/Maccretor value for helium main sequence stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_HeHG": {"param_name": "qcrit_degenerate_HeHG", "description": "Apply critical q=Mdonor/Maccretor value for helium Hertzsprung gap stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_HeGB": {"param_name": "qcrit_degenerate_HeGB", "description": "Apply critical q=Mdonor/Maccretor value for helium red giant stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_HeWD": {"param_name": "qcrit_degenerate_HeWD", "description": "Apply critical q=Mdonor/Maccretor value for helium white dwarf stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_COWD": {"param_name": "qcrit_degenerate_COWD", "description": "Apply critical q=Mdonor/Maccretor value for carbon-oxygen white dwarf stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_ONeWD": {"param_name": "qcrit_degenerate_ONeWD", "description": "Apply critical q=Mdonor/Maccretor value for oxygen-neon white dwarf stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_NS": {"param_name": "qcrit_degenerate_NS", "description": "Apply critical q=Mdonor/Maccretor value for neutron stars to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "qcrit_degenerate_BH": {"param_name": "qcrit_degenerate_BH", "description": "Apply critical q=Mdonor/Maccretor value for black holes to determine the stability of Roche-lobe overflow for degenerate accretors. See also qcrits_*, qcrits_degenerate_*.", "rest": "(null)"}, "mass_for_Hestar_Ia_upper": {"param_name": "mass_for_Hestar_Ia_upper", "description": "Only helium stars below this mass can explode as SNIa. Default is zero, i.e. it never happens. See also mass_for_Hestar_Ia_lower.", "rest": "(null)"}, "mass_for_Hestar_Ia_lower": {"param_name": "mass_for_Hestar_Ia_lower", "description": "Only helium stars above this mass can explode as SNIa. Default is zero, i.e. it never happens. See also mass_for_Hestar_Ia_upper.", "rest": "(null)"}, "alphaCB": {"param_name": "alphaCB", "description": "Circumbinary disk viscosity parameter, alpha.", "rest": "(null)"}, "minimum_donor_menv_for_comenv": {"param_name": "minimum_donor_menv_for_comenv", "description": "Minimum donor envelope mass for common envelope evolution to be triggered (Msun). Default 0.", "rest": "(null)"}, "comenv_prescription": {"param_name": "comenv_prescription", "description": "Use this to choose which common envelope prescription you should use. 0=Hurley et al 2002 (based on the Paczy\u0144ski energy model) or 1=Nelemans and Tout (angular momentum model). See also alpha_ce, comenv_ms_accretion_mass, comenv_ms_accretion_fraction, comenv_ns_accretion_fraction, comenv_ns_accretion_mass, nelemans_gamma, nelemans_minq, nelemans_max_frac_j_change, nelemans_n_comenvs, lambda_ce, lambda_ionisation.", "rest": "(null)"}, "comenv_prescription%d": {"param_name": "comenv_prescription%d", "description": "Use this to choose which common envelope prescription you should use. 0=Hurley et al 2002 (based on the Paczy\u0144ski energy model) or 1=Nelemans and Tout (angular momentum model). See also alpha_ce, comenv_ms_accretion_mass, comenv_ms_accretion_fraction, comenv_ns_accretion_fraction, comenv_ns_accretion_mass, nelemans_gamma, nelemans_minq, nelemans_max_frac_j_change, nelemans_n_comenvs, lambda_ce, lambda_ionisation.", "rest": "(null)"}, "comenv_ejection_spin_method": {"param_name": "comenv_ejection_spin_method", "description": "When a common envelope is ejected, we need to decide how fast the stars are left spinning. COMENV_EJECTION_SPIN_METHOD_DO_NOTHING (0) is the default, this just leaves the stars/stellar cores spinning with the same spin rate (omega = angular velocity) with which they entered the common envelope phase. COMENV_EJECTION_SPIN_METHOD_SYCHRONIZE instead tidally synchronizes the stars with their new orbital angular velocity.", "rest": "(null)"}, "comenv_merger_spin_method": {"param_name": "comenv_merger_spin_method", "description": "When a common envelope binary merges, we need to decide how fast the resulting single star is left spinning. COMENV_MERGER_SPIN_METHOD_SPECIFIC (0) is the default, this preserves angular momentum but limits the specific angular momentum of the merged star to the specific angular momentum of the system at the onset of common envelope evolution. COMENV_MERGER_SPIN_METHOD_CONSERVE_ANGMOM (1) sets the merger's angular momentum to be that of the system at the onset of common envelope evolution (which means the star may be rotating supercritically). COMENV_MERGER_SPIN_METHOD_CONSERVE_OMEGA (2) sets the spin rate (angular frequency = omega) of the merged star to be that of the orbit just at the onset of common envelope evolution.", "rest": "(null)"}, "comenv_ms_accretion_mass": {"param_name": "comenv_ms_accretion_mass", "description": "Experimental. During common envelope evolution, a main sequence star may accrete some of the envelope's mass. Requires COMENV_MS_ACCRETION. See also comenv_ms_accretion_fraction.", "rest": "(null)"}, "comenv_ms_accretion_fraction": {"param_name": "comenv_ms_accretion_fraction", "description": "Experimental. During common envelope evolution, a main sequence may accrete a fraction of the envelope's mass. Requires COMENV_MS_ACCRETION. See also comenv_ms_accretion_mass.", "rest": "(null)"}, "comenv_ns_accretion_mass": {"param_name": "comenv_ns_accretion_mass", "description": "Experimental. During common envelope evolution, a neutron star may accrete some of the envelope's mass. Requires COMENV_NS_ACCRETION. See also comenv_ns_accretion_fraction.", "rest": "(null)"}, "comenv_ns_accretion_fraction": {"param_name": "comenv_ns_accretion_fraction", "description": "Experimental. During common envelope evolution, a neutron star may accrete a fraction of the envelope's mass. Requires COMENV_NS_ACCRETION. See also comenv_ns_accretion_mass.", "rest": "(null)"}, "alpha_ce": {"param_name": "alpha_ce", "description": "Common envelope energy formalism parameter. A fraction alpha of the orbital energy is used to eject the envelope. See Hurley et al 2002 for details.", "rest": "(null)"}, "alpha_ce%d": {"param_name": "alpha_ce%d", "description": "Common envelope energy formalism parameter. A fraction alpha of the orbital energy is used to eject the envelope. See Hurley et al. 2002 for details.", "rest": "(null)"}, "lambda_ce": {"param_name": "lambda_ce", "description": "Common envelope parameter. The binding energy of the common envelope is G*M*Menv/(lambda*R). Typically this is taken to be 0.5, but if set to LAMBDA_CE_DEWI_TAURIS == -1 binary_c uses the Dewi and Tauris fits instead, LAMBDA_CE_WANG_2016 == -2 uses the formalism of Wang, Jia and Li (2016), if LAMBDA_CE_POLYTROPE == -3 then a polytropic formalism is used (see also comenv_splitmass) and if LAMBDA_CE_KLENCKI_2020 == -4 use Klencki et al. (2020).", "rest": "(null)"}, "lambda_ce%d": {"param_name": "lambda_ce%d", "description": "Common envelope parameter. The binding energy of the common envelope is G*M*Menv/(lambda*R). Typically this is taken to be 0.5, but if set to -1 binary_c uses the Dewi and Tauris fits instead, -2 uses the formalism of Wang, Jia and Li (2016) and if -3 then a polytropic formalism is used (see also comenv_splitmass).", "rest": "(null)"}, "comenv_splitmass": {"param_name": "comenv_splitmass", "description": "When lambda_ce=-2, the envelope binding energy, lambda, is calculated using a polytropic formalism. The comenv_splitmass defines the point, in the units of the core mass, above which material is ejected.", "rest": "(null)"}, "nelemans_recalc_eccentricity": {"param_name": "nelemans_recalc_eccentricity", "description": "If True, recalculate the eccentricity after angular momentum is removed. ", "rest": "(null)"}, "comenv_post_eccentricity": {"param_name": "comenv_post_eccentricity", "description": "Eccentricity remaining after common envelope ejection.", "rest": "(null)"}, "dedmRLOF": {"param_name": "dedmRLOF", "description": "de/dM during RLOF (defualt 0.0)", "rest": "(null)"}, "nelemans_gamma": {"param_name": "nelemans_gamma", "description": "Set the fraction of the orbital specific angular momentum that is used to eject the common envelope according to the Nelemans and Tout prescription. See also nelemans_minq, nelemans_max_frac_j_change, nelemans_n_comenvs.", "rest": "(null)"}, "nelemans_minq": {"param_name": "nelemans_minq", "description": "Only activate the Nelemans and Tout common envelope prescription for q>nelemans_minq. See also nelemans_gamma, nelemans_max_frac_j_change, nelemans_n_comenvs.", "rest": "(null)"}, "nelemans_max_frac_j_change": {"param_name": "nelemans_max_frac_j_change", "description": "Maximum fractional angular momentum change in the Nelemans and Tout common envelope prescription. See also nelemans_gamma, nelemans_minq, nelemans_n_comenvs.", "rest": "(null)"}, "nelemans_n_comenvs": {"param_name": "nelemans_n_comenvs", "description": "Set the maximum number of common envelope ejections allowed to follow the Nelemans and Tout prescription, after which the standard alpha prescription is used.", "rest": "(null)"}, "lambda_ionisation": {"param_name": "lambda_ionisation", "description": "A fraction lambda_ionisation of the recombination energy in the common envelope goes into ejecting the envelope. This is usually 0.0, but a positive value can make a big difference to the outcome of common envelope evolution.", "rest": "(null)"}, "lambda_ionisation%d": {"param_name": "lambda_ionisation%d", "description": "A fraction lambda_ionisation of the recombination energy in the common envelope goes into ejecting the envelope. This is usually 0.0, but a positive value can make a big difference to the outcome of common envelope evolution.", "rest": "(null)"}, "lambda_enthalpy": {"param_name": "lambda_enthalpy", "description": "A fraction of the enthalpy to be included in the common envelope evolution binding energy. Only used for the Wang 2016 prescription (so far).", "rest": "(null)"}, "lambda_enthalpy%d": {"param_name": "lambda_enthalpy%d", "description": "A fraction of the enthalpy to be included in the common envelope evolution binding energy. Only used for the Wang 2016 prescription (so far).", "rest": "(null)"}, "cbdisc_albedo": {"param_name": "cbdisc_albedo", "description": "Circumbinary-disc albedo. Requires DISCS.", "rest": "(null)"}, "cbdisc_gamma": {"param_name": "cbdisc_gamma", "description": "Circumbinary disc gamma (equation of state) parameter. Requires DISCS.", "rest": "(null)"}, "cbdisc_alpha": {"param_name": "cbdisc_alpha", "description": "Circumbinary disc alpha (viscosity) parameter. Requires DISCS.", "rest": "(null)"}, "cbdisc_kappa": {"param_name": "cbdisc_kappa", "description": "Circumbinary disc kappa (opacity) parameter. Requires DISCS.", "rest": "(null)"}, "cbdisc_minimum_evaporation_timescale": {"param_name": "cbdisc_minimum_evaporation_timescale", "description": "Circumbinary disc minimum evaporation timescale (years). If (slow, not edge stripped) mass loss would evaporate the disc on a timescale less than this, simply evaporate the disc immediated. Usually set to 1y, ignore if zero. Requires DISCS.", "rest": "(null)"}, "cbdisc_torquef": {"param_name": "cbdisc_torquef", "description": "Circumbinary disc binary torque multiplier. Requires DISCS.", "rest": "(null)"}, "cbdisc_max_lifetime": {"param_name": "cbdisc_max_lifetime", "description": "Circumbinary disc maximum lifetime (years, ignored if 0). Requires DISCS.", "rest": "(null)"}, "cbdisc_init_dM": {"param_name": "cbdisc_init_dM", "description": "On cbdisc start, reduce mass by a fraction dM if it won't converge. Requires DISCS.", "rest": "(null)"}, "cbdisc_init_dJdM": {"param_name": "cbdisc_init_dJdM", "description": "On cbdisc start, reduce angular momentum by a fraction dJ/dM*dM if it won't converge. Requires DISCS.", "rest": "(null)"}, "cbdisc_mass_loss_constant_rate": {"param_name": "cbdisc_mass_loss_constant_rate", "description": "Circumbinary disc constant mass loss rate (Msun/year). Requires DISCS.", "rest": "(null)"}, "cbdisc_mass_loss_FUV_multiplier": {"param_name": "cbdisc_mass_loss_FUV_multiplier", "description": "Circumbinary disc FUV mass loss rate multiplier (no units). Requires DISCS.", "rest": "(null)"}, "cbdisc_mass_loss_Xray_multiplier": {"param_name": "cbdisc_mass_loss_Xray_multiplier", "description": "Circumbinary disc X-ray mass loss rate multiplier (no units). Requires DISCS.", "rest": "(null)"}, "cbdisc_mass_loss_ISM_ram_pressure_multiplier": {"param_name": "cbdisc_mass_loss_ISM_ram_pressure_multiplier", "description": "Circumbinary disc interstellar medium ram pressure stripping mass loss rate multiplier (no units). Requires DISCS.", "rest": "(null)"}, "cbdisc_mass_loss_ISM_pressure": {"param_name": "cbdisc_mass_loss_ISM_pressure", "description": "Circumbinary disc interstellar medium ram pressure in units of Boltzmann constant per Kelvin (I think...). Requires DISCS. Typically 3000.0. See e.g. http://www.astronomy.ohio-state.edu/~pogge/Ast871/Notes/Intro.pdf page 15 or https://arxiv.org/pdf/0902.0820.pdf Fig. 1 (left panel).", "rest": "(null)"}, "cbdisc_mass_loss_inner_viscous_multiplier": {"param_name": "cbdisc_mass_loss_inner_viscous_multiplier", "description": "Circumbinary disc inner edge viscous mass loss rate multiplier (no units). Requires DISCS.", "rest": "(null)"}, "cbdisc_mass_loss_inner_viscous_angular_momentum_multiplier": {"param_name": "cbdisc_mass_loss_inner_viscous_angular_momentum_multiplier", "description": "Circumbinary disc inner edge viscous angular momentum multiplier (no units). The inner edge angular momentum Requires DISCS.", "rest": "(null)"}, "cbdisc_resonance_multiplier": {"param_name": "cbdisc_resonance_multiplier", "description": "Circumbinary disc resonant interaction multiplier, affects eccentricity pumping and angular momentum rates. Requires DISCS.", "rest": "(null)"}, "cbdisc_resonance_damping": {"param_name": "cbdisc_resonance_damping", "description": "Circumbinary disc resonant interaction damping: should be on (True) to damp the l=1, m=2 resonance when the disc inner edge lies outside the resonance location. Requires DISCS.", "rest": "(null)"}, "cbdisc_fail_ring_inside_separation": {"param_name": "cbdisc_fail_ring_inside_separation", "description": "If True, while converging on a structure, circumbinary discs with Rring < the binary separation are immediately failed.", "rest": "(null)"}, "cbdisc_mass_loss_inner_L2_cross_multiplier": {"param_name": "cbdisc_mass_loss_inner_L2_cross_multiplier", "description": "Circumbinary disc inner edge L2-crossing mass loss rate multiplier (no units). Requires DISCS.", "rest": "(null)"}, "cbdisc_minimum_luminosity": {"param_name": "cbdisc_minimum_luminosity", "description": "Circumbinary disc minimum luminosity. If the disc becomes dimmer than this, the disc is evaporated instantly. Requires DISCS.", "rest": "(null)"}, "cbdisc_minimum_mass": {"param_name": "cbdisc_minimum_mass", "description": "Circumbinary disc minimum mass. If the disc becomes less massive than this, the disc is evaporated instantly. Requires DISCS.", "rest": "(null)"}, "cbdisc_minimum_fRing": {"param_name": "cbdisc_minimum_fRing", "description": "Circumbinary disc minimum fRing. If the disc becomes a ring, and fRing = |Rout/Rin-1| < this value (and this value is non-zero), the disc is evaporated instantly. Requires DISCS.", "rest": "(null)"}, "comenv_disc_angmom_fraction": {"param_name": "comenv_disc_angmom_fraction", "description": "If >0 Fraction of the common envelope's angular momentum that goes into the circumbinary disc. If -1 then uses the moments of inertia to calculate (deprecated), if -2 use the common envelope's specific angular momentum, if -3 uses the L2 point at the end of the common envelope to set the angular momentum. Requires DISCS and DISCS_CIRCUMBINARY_FROM_COMENV.", "rest": "(null)"}, "comenv_disc_mass_fraction": {"param_name": "comenv_disc_mass_fraction", "description": "Fraction of the common envelope's mass that goes into the circumbinary disc. Requires DISCS and DISCS_CIRCUMBINARY_FROM_COMENV.", "rest": "(null)"}, "wind_disc_angmom_fraction": {"param_name": "wind_disc_angmom_fraction", "description": "If >0 Fraction of the wind envelope's angular momentum that goes into the circumbinary disc. If -1 then uses the L2 point's specific angular momentum. Requires DISCS and DISCS_CIRCUMBINARY_FROM_WIND.", "rest": "(null)"}, "wind_disc_mass_fraction": {"param_name": "wind_disc_mass_fraction", "description": "Fraction of the stellar wind's mass that goes into the circumbinary disc. Requires DISCS and DISCS_CIRCUMBINARY_FROM_WIND.", "rest": "(null)"}, "WRLOF_method": {"param_name": "WRLOF_method", "description": "Choose whether and how to apply wind-Roche-lobe-overflow. 0=none, 1=q-dependent, 2=quadratic See Abate et al 2013/14 for details. Requires WRLOF_MASS_TRANSFER.", "rest": "(null)"}, "minimum_timestep": {"param_name": "minimum_timestep", "description": "The minimum timestep (Myr).", "rest": "(null)"}, "timestep_solver_factor": {"param_name": "timestep_solver_factor", "description": "Factor applied in timestep_limits, e.g. to prevent X changing too fast by comparing to X/dX/dt, which is usually 1 but can be higher to lengthen timesteps when using an alternative solver.", "rest": "(null)"}, "RLOF_mdot_factor": {"param_name": "RLOF_mdot_factor", "description": "Multiplier applied to the mass transfer rate during Roche-lobe overflow. Requires RLOF_MDOT_MODULATION.", "rest": "(null)"}, "RLOF_f": {"param_name": "RLOF_f", "description": "Factor to enlarge a Roche lobe, nominally because of radiation pressure (see Dermine et al paper). Requires RLOF_RADIATION_CORRECTION.", "rest": "(null)"}, "unstable_RLOF_can_trigger_SNIa": {"param_name": "unstable_RLOF_can_trigger_SNIa", "description": "If true, allow unstable (dynamical) RLOF to trigger a sub-MCh SNIa. (False)", "rest": "(null)"}, "triggered_SNIa_algorithm": {"param_name": "triggered_SNIa_algorithm", "description": "Algorithm to use for triggered SNeIa", "rest": "(null)"}, "minimum_separation_for_instant_RLOF": {"param_name": "minimum_separation_for_instant_RLOF", "description": "If True, instead of evolving the system just report the minimum separation (on the zero-age main sequence) that would lead to instant RLOF. Used by binary_grid. See also minimum_orbital_period_for_instant_RLOF and maximum_mass_ratio_for_instant_RLOF.", "rest": "(null)"}, "minimum_orbital_period_for_instant_RLOF": {"param_name": "minimum_orbital_period_for_instant_RLOF", "description": "If True, instead of evolving the system just report the minimum orbital period (on the zero-age main sequence) that would lead to instant RLOF. Used by binary_grid. See also minimum_separation_for_instant_RLOF and maximum_mass_ratio_for_instant_RLOF.", "rest": "(null)"}, "maximum_mass_ratio_for_instant_RLOF": {"param_name": "maximum_mass_ratio_for_instant_RLOF", "description": "If True, instead of evolving the system just report the maximum mass ratio (on the zero-age main sequence) that would lead to instant RLOF, given M1 and orbital period. Used by binary_grid. See also minimum_separation_for_instant_RLOF and minimum_orbital_period_for_instant_RLOF.", "rest": "(null)"}, "RLOF_method": {"param_name": "RLOF_method", "description": "Use RLOF_method to choose the algorithm you use for Roche-lobe overflow mass loss rate calculations. 0=Hurley et al 2002, 1=Adaptive (for radiative stars) R=RL method, 2=Ritter (probably broken), 3=Claeys etal 2014 variant on Hurley et al 2002.", "rest": "(null)"}, "RLOF_interpolation_method": {"param_name": "RLOF_interpolation_method", "description": "When a star overflows its Roche lobe, it always has R>RL because of the limited time resolution of the simulation. Binary_c then uses an algorithm to get back to when R~RL (within a desired tolerance, set in RLOF_ENTRY_THRESHOLD which is usually 1.02, i.e. overflow of 2%). You can choose algorithm 0, the Hurley et al 2002 method which reverses time (i.e. uses a Newton-like scheme), or 1 to use the binary_c method which rejects a timestep (and hence does no logging on that timestep) and repeats with half the timestep until R~RL. The latter is now the default, because this means there are no negative timesteps which break various other algorithms (e.g. nucleosynthesis).", "rest": "(null)"}, "He_nova_ELDs": {"param_name": "He_nova_ELDs", "description": "Enable edge-lit detonations from WDs that have He novae. (Default: False, i.e. off.)", "rest": "(null)"}, "nova_retention_fraction_H": {"param_name": "nova_retention_fraction_H", "description": "The mass accreted during a hydrogen nova as fraction of mass transferred.", "rest": "(null)"}, "nova_retention_fraction_He": {"param_name": "nova_retention_fraction_He", "description": "The mass accreted during a helium nova as fraction of mass transferred.", "rest": "(null)"}, "beta_reverse_nova": {"param_name": "beta_reverse_nova", "description": "The fraction of mass ejected in a nova explosion which is accreted back onto the companion star. Set to -1 to automatically calculate based on a geometric argument, or 0 or positive to set the value.", "rest": "(null)"}, "WD_accretion_rate_nalgorithms": {"param_name": "WD_accretion_rate_nalgorithms", "description": "Wrapper to set all WD accretion rates in one go (see WD_accretion_rate_*).", "rest": "(null)"}, "WD_accretion_rate_novae_upper_limit_hydrogen_donor": {"param_name": "WD_accretion_rate_novae_upper_limit_hydrogen_donor", "description": "Upper limit of the stable mass transfer rate onto a white dwarf that leads to novae when the donor is hydrogen rich: above this rate the mass transfer leads to stable burning.", "rest": "(null)"}, "WD_accretion_rate_novae_upper_limit_helium_donor": {"param_name": "WD_accretion_rate_novae_upper_limit_helium_donor", "description": "Upper limit of the stable mass transfer rate onto a white dwarf that leads to novae when the donor is helium rich: above this rate the mass transfer leads to stable burning.", "rest": "(null)"}, "WD_accretion_rate_novae_upper_limit_other_donor": {"param_name": "WD_accretion_rate_novae_upper_limit_other_donor", "description": "Upper limit of the stable mass transfer rate onto a white dwarf that leads to novae when the donor is neither hydrogen nor helium rich: above this rate the mass transfer leads to stable burning.", "rest": "(null)"}, "WD_accretion_rate_new_giant_envelope_lower_limit_hydrogen_donor": {"param_name": "WD_accretion_rate_new_giant_envelope_lower_limit_hydrogen_donor", "description": "Lower limit of the mass transfer rate onto a white dwarf that leads to a the formation of a new giant envelope with a hydrogen-rich donor. Below this mass transfer leads to stable burning.", "rest": "(null)"}, "WD_accretion_rate_new_giant_envelope_lower_limit_helium_donor": {"param_name": "WD_accretion_rate_new_giant_envelope_lower_limit_helium_donor", "description": "Lower limit of the mass transfer rate onto a white dwarf that leads to a the formation of a new giant envelope with a helium-rich donor. Below this mass transfer leads to stable burning.", "rest": "(null)"}, "WD_accretion_rate_new_giant_envelope_lower_limit_other_donor": {"param_name": "WD_accretion_rate_new_giant_envelope_lower_limit_other_donor", "description": "Lower limit of the mass transfer rate onto a white dwarf that leads to a the formation of a new giant envelope when the donor is neither hydrogen nor helium rich. Below this mass transfer leads to stable burning.", "rest": "(null)"}, "CRAP_parameter": {"param_name": "CRAP_parameter", "description": "Tidally enhanced mass loss parameter. See Tout and Eggleton's paper on the subject. (Was the parameter bb).", "rest": "(null)"}, "individual_novae": {"param_name": "individual_novae", "description": "If individual_novae is True, novae are resolved such that each explosion is performed separtaely.", "rest": "(null)"}, "nova_timestep_accelerator_num": {"param_name": "nova_timestep_accelerator_num", "description": "The nova timestep is accelerated if the nova number exceeds nova_timestep_accelerator_num. If zero or negative, acceleration is off. See also nova_timestep_accelerator_index and nova_timestep_accelerator_max. Only used if individual_novae is on.", "rest": "(null)"}, "nova_timestep_accelerator_index": {"param_name": "nova_timestep_accelerator_index", "description": "The index at which the nova timestep is accelerated. A larger value gives longer timesteps. See also nova_timestep_accelerator_num and nova_timestep_accelerator_max. Only used if individual_novae is on.", "rest": "(null)"}, "nova_timestep_accelerator_max": {"param_name": "nova_timestep_accelerator_max", "description": "The nova timestep is accelerated by a factor that is capped at nova_timestep_accelerator_max. This parameter is ignored if it is zero or negative. See also nova_timestep_accelerator_num and nova_timestep_accelerator_index. Only used if individual_novae is on.", "rest": "(null)"}, "eccentric_RLOF_model": {"param_name": "eccentric_RLOF_model", "description": "Chooses which model is used to handle eccentric RLOF. Default is RLOF_ECCENTRIC_AS_CIRCULAR, i.e. ignore the eccentricity. Note: requires force_corotation_of_primary_and_orbit to be FALSE.", "rest": "(null)"}, "force_circularization_on_RLOF": {"param_name": "force_circularization_on_RLOF", "description": "If True forces circularization of stars and orbit when RLOF starts, this is as in the BSE algorithm. (True)", "rest": "(null)"}, "resolve_stellar_type_changes": {"param_name": "resolve_stellar_type_changes", "description": "If True forces binary_c to resolve stellar type changes to within the minimum timestep. Warning: can be slow. (True)", "rest": "(null)"}, "nonconservative_angmom_gamma": {"param_name": "nonconservative_angmom_gamma", "description": "Mass lost from the system (but NOT from a stellar wind) takes a fraction gamma of the orbital angular momentum with it. Set to -1 to take the specific angular momentum of the donor star. Set to -2 to take super-Eddington, nova and disk-wind angular momenta as if a wind from the accretor.", "rest": "(null)"}, "max_stellar_angmom_change": {"param_name": "max_stellar_angmom_change", "description": "Maxmimum fractional change in stellar angular momentum allowed before a timestep is rejected (0.05).", "rest": "(null)"}, "id_number": {"param_name": "id_number", "description": "Set the integer ID number of the system", "rest": "0"}, "decretion_disc_radius_algorithm": {"param_name": "decretion_disc_radius_algorithm", "description": "Decretion disc radius calculation algorithm. ", "rest": "0"}, "system_list": {"param_name": "system_list", "description": "Set the path to the a system_list file which has a list of arguments on each line.", "rest": ""}, "core_collapse_energy": {"param_name": "core_collapse_energy", "description": "Set algorithm for computation of the energy of a core-collapse supernova. 0 = CORE_COLLAPSE_ENERGY_ONE_FOE = always 10^51 erg. 1 = CORE_COLLAPSE_ENERGY_MARASSI2019 use data from Marassi et al. (2019).", "rest": "0"}, "baryonic_to_gravitational_remnant_mass_prescription": {"param_name": "baryonic_to_gravitational_remnant_mass_prescription", "description": "Baryonic to gravitational remnant mass prescription. During the collapse of a massive star the proto-compact object loses mass through neutrino emission.", "rest": "0"}}}, "nucsyn": {"section_name": "nucsyn", "parameters": {"third_dup": {"param_name": "third_dup", "description": "If True, enables third dredge up. Requires NUCSYN and NUCSYN_THIRD_DREDGE_UP.", "rest": "(null)"}, "third_dup_multiplier": {"param_name": "third_dup_multiplier", "description": "Usage: --third_dup_multiplier <i> <f>. Multiplies the abundance of element <i> by <f> during third dredge up.", "rest": "1.0"}, "NeNaMgAl": {"param_name": "NeNaMgAl", "description": "Enables NeNaMgAl reaction network. Requires NUCSYN and NUCSYN_HBB.", "rest": "Ignore"}, "nucsyn_network%d": {"param_name": "nucsyn_network%d", "description": "Usage: --nucsyn_network%d <boolean>. Turn a nuclear network on or off.", "rest": "(null)"}, "nucsyn_network_error%d": {"param_name": "nucsyn_network_error%d", "description": "Usage: --nucsyn_network_error%d <f>. Threshold error in nuclear network solver for network %d.", "rest": "(null)"}, "nucreacmult%d": {"param_name": "nucreacmult%d", "description": "Usage: --nucreacmult%d <f>. Multiply nuclear reaction given by the integer %d (integer) by f (float). ", "rest": "(null)"}, "nucsyn_metallicity": {"param_name": "nucsyn_metallicity", "description": "This sets the metallicity of the nucleosynthesis algorithms, i.e. the amount (by mass) of matter which is not hydrogen or helium. Usually you'd just set this with the metallicity parameter, but if you want the nucleosynthesis to be outside the range of the stellar evolution algorithm (e.g. Z=0 or Z=0.04) then you need to use nucsyn_metallicity. That said, it's also outside the range of some of the nucleosynthesis algorithms as well, so you have been warned!", "rest": "(null)"}, "nucsyn_solver": {"param_name": "nucsyn_solver", "description": "Choose the solver used in nuclear burning. 0 = KAPS_RENTROP is a Kaps-Rentrop scheme (fast, not great for stiff problems), 1 = LSODA (Adams/BSF switcher), 2 = CVODE library (https://computing.llnl.gov/projects/sundials. Default 0. ", "rest": "0"}, "initial_abundance_mix": {"param_name": "initial_abundance_mix", "description": "initial abundance mixture: 0=AG89, 1=Karakas 2002, 2=Lodders 2003, 3=Asplund 2005 (not available?), 4=Garcia Berro, 5=Grevesse Noels 1993", "rest": "0"}, "init_abund": {"param_name": "init_abund", "description": "Usage: --init_abund <i> <X>. Sets the initial abundance of isotope number <i> to mass fraction <X>.", "rest": "0.02"}, "init_abund_mult": {"param_name": "init_abund_mult", "description": "Usage: --init_abund_mult <i> <f>. Multiplies the initial abundance of isotope number <i> by <f>.", "rest": "1.0"}, "init_abund_dex": {"param_name": "init_abund_dex", "description": "Usage: --init_abund_dex <i> <f>. Changes the initial abundance of isotope number <i> by <f> dex.", "rest": "0.0"}, "init_abunds_only": {"param_name": "init_abunds_only", "description": "If True, outputs only the initial abundances, then exits.", "rest": "(null)"}, "initial_abunds_only": {"param_name": "initial_abunds_only", "description": "If True, outputs only the initial abundances, then exits.", "rest": "(null)"}, "no_thermohaline_mixing": {"param_name": "no_thermohaline_mixing", "description": "If True, disables thermohaline mixing.", "rest": "(null)"}, "lithium_GB_post_Heflash": {"param_name": "lithium_GB_post_Heflash", "description": "Sets the lithium abundances after the helium flash. Requires NUCSYN and LITHIUM_TABLES.", "rest": "(null)"}, "lithium_GB_post_1DUP": {"param_name": "lithium_GB_post_1DUP", "description": "Sets the lithium abundance after first dredge up. Requires NUCSYN and LITHIUM_TABLES.", "rest": "(null)"}, "lithium_hbb_multiplier": {"param_name": "lithium_hbb_multiplier", "description": "Multiplies the lithium abundances on the AGB during HBB (based on Karakas/Fishlock et al models).Requires NUCSYN and LITHIUM_TABLES.", "rest": "(null)"}, "angelou_lithium_decay_function": {"param_name": "angelou_lithium_decay_function", "description": "Functional form which describes Li7 decay. Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Choices are: 0 expoential (see angelou_lithium_decay_time).", "rest": "(null)"}, "angelou_lithium_LMMS_time": {"param_name": "angelou_lithium_LMMS_time", "description": "Time at which lithium manufacture is triggered in a low-mass (convective) main sequence (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_MS_time": {"param_name": "angelou_lithium_MS_time", "description": "Time at which lithium manufacture is triggered on the main sequence (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_HG_time": {"param_name": "angelou_lithium_HG_time", "description": "Time at which lithium manufacture is triggered on the Hertzsprung gap (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_GB_time": {"param_name": "angelou_lithium_GB_time", "description": "Time at which lithium manufacture is triggered on the giant branch (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_CHeB_time": {"param_name": "angelou_lithium_CHeB_time", "description": "Time at which lithium manufacture is triggered during core helium burning (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_EAGB_time": {"param_name": "angelou_lithium_EAGB_time", "description": "Time at which lithium manufacture is triggered on the early AGB (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_TPAGB_time": {"param_name": "angelou_lithium_TPAGB_time", "description": "Time at which lithium manufacture is triggered on the thermally pulsing AGB (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_LMMS_decay_time": {"param_name": "angelou_lithium_LMMS_decay_time", "description": "Decay time for surface lithium abundance during the low-mass (convective) main sequence (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_MS_decay_time": {"param_name": "angelou_lithium_MS_decay_time", "description": "Decay time for surface lithium abundance on the main sequence (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_HG_decay_time": {"param_name": "angelou_lithium_HG_decay_time", "description": "Decay time for surface lithium abundance on the Hertzsprung gap (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_GB_decay_time": {"param_name": "angelou_lithium_GB_decay_time", "description": "Decay time for surface lithium abundance on the giant branch (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_CHeB_decay_time": {"param_name": "angelou_lithium_CHeB_decay_time", "description": "Decay time for surface lithium abundance during core helium burning (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_EAGB_decay_time": {"param_name": "angelou_lithium_EAGB_decay_time", "description": "Decay time for surface lithium abundance on the early AGB (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_TPAGB_decay_time": {"param_name": "angelou_lithium_TPAGB_decay_time", "description": "Decay time for surface lithium abundance on the thermally pulsing AGB (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_LMMS_massfrac": {"param_name": "angelou_lithium_LMMS_massfrac", "description": "Lithium mass fraction when its manufacture is triggered during the low-mass (convective) main sequence (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_MS_massfrac": {"param_name": "angelou_lithium_MS_massfrac", "description": "Lithium mass fraction when its manufacture is triggered on the main sequence (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_HG_massfrac": {"param_name": "angelou_lithium_HG_massfrac", "description": "Lithium mass fraction when its manufacture is triggered on the Hertzsprung gap (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_GB_massfrac": {"param_name": "angelou_lithium_GB_massfrac", "description": "Lithium mass fraction when its manufacture is triggered on the giant branch (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_CHeB_massfrac": {"param_name": "angelou_lithium_CHeB_massfrac", "description": "Lithium mass fraction when its manufacture is triggered during core helium burning (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_EAGB_massfrac": {"param_name": "angelou_lithium_EAGB_massfrac", "description": "Lithium mass fraction when its manufacture is triggered on the early AGB (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_TPAGB_massfrac": {"param_name": "angelou_lithium_TPAGB_massfrac", "description": "Lithium mass fraction when its manufacture is triggered on the thermally pulsing AGB (Myr). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0 (for the start, use 1e-6).", "rest": "(null)"}, "angelou_lithium_vrot_trigger": {"param_name": "angelou_lithium_vrot_trigger", "description": "Equatorial rotational velocity at which lithium manufacture is triggered (km/s). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0.", "rest": "(null)"}, "angelou_lithium_vrotfrac_trigger": {"param_name": "angelou_lithium_vrotfrac_trigger", "description": "Fraction of Keplerian (breakup) equatorial rotational velocity at which lithium manufacture is triggered (must be <1, ignored if 0). Requires NUCSYN and NUCSYN_ANGELOU_LITHIUM. Ignored if 0.", "rest": "(null)"}}}, "output": {"section_name": "output", "parameters": {"cf_amanda_log": {"param_name": "cf_amanda_log", "description": "Enable logging to compare to Amanda's models.", "rest": "(null)"}, "float_overflow_checks": {"param_name": "float_overflow_checks", "description": "Turn on to enable floating-point overflow checks at the end of each timestep, if they are available. 0=off, 1=warn (stderr) on failure, 2=exit on failure (0)", "rest": "(null)"}, "save_pre_events_stardata": {"param_name": "save_pre_events_stardata", "description": "Enable this to save a copy of stardata to stardata->pre_events_stardata just before an event.", "rest": "(null)"}, "disable_end_logging": {"param_name": "disable_end_logging", "description": "Disable the logging that happens at the end of the evolution.", "rest": "(null)"}, "ensemble": {"param_name": "ensemble", "description": "Turn on ensemble calculations and output.", "rest": "(null)"}, "ensemble_filters_off": {"param_name": "ensemble_filters_off", "description": "Sets all ensemble filters to be off (FALSE) - these can then be enabled one-by-one with --ensemble_filter_[...] TRUE.", "rest": "(null)"}, "ensemble_filter_%d": {"param_name": "ensemble_filter_%d", "description": "Turn on or off ensemble filter <n>. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_SCALARS": {"param_name": "ensemble_filter_SCALARS", "description": "Turn on or off ensemble filter SCALARS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_HRD": {"param_name": "ensemble_filter_HRD", "description": "Turn on or off ensemble filter HRD. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_SUPERNOVAE": {"param_name": "ensemble_filter_SUPERNOVAE", "description": "Turn on or off ensemble filter SUPERNOVAE. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_CHEMICALLY_PECULIAR": {"param_name": "ensemble_filter_CHEMICALLY_PECULIAR", "description": "Turn on or off ensemble filter CHEMICALLY_PECULIAR. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_SPECTRAL_TYPES": {"param_name": "ensemble_filter_SPECTRAL_TYPES", "description": "Turn on or off ensemble filter SPECTRAL_TYPES. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_INITIAL_DISTRIBUTIONS": {"param_name": "ensemble_filter_INITIAL_DISTRIBUTIONS", "description": "Turn on or off ensemble filter INITIAL_DISTRIBUTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_TEST": {"param_name": "ensemble_filter_TEST", "description": "Turn on or off ensemble filter TEST. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_ORBIT": {"param_name": "ensemble_filter_ORBIT", "description": "Turn on or off ensemble filter ORBIT. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_MASS_FUNCTIONS": {"param_name": "ensemble_filter_MASS_FUNCTIONS", "description": "Turn on or off ensemble filter MASS_FUNCTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_LUMINOSITY_FUNCTIONS": {"param_name": "ensemble_filter_LUMINOSITY_FUNCTIONS", "description": "Turn on or off ensemble filter LUMINOSITY_FUNCTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_VEQ_FUNCTIONS": {"param_name": "ensemble_filter_VEQ_FUNCTIONS", "description": "Turn on or off ensemble filter VEQ_FUNCTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_MERGED": {"param_name": "ensemble_filter_MERGED", "description": "Turn on or off ensemble filter MERGED. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_STELLAR_TYPE_COUNTS": {"param_name": "ensemble_filter_STELLAR_TYPE_COUNTS", "description": "Turn on or off ensemble filter STELLAR_TYPE_COUNTS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_CHEMICAL_YIELDS": {"param_name": "ensemble_filter_CHEMICAL_YIELDS", "description": "Turn on or off ensemble filter CHEMICAL_YIELDS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_EMP": {"param_name": "ensemble_filter_EMP", "description": "Turn on or off ensemble filter EMP. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_CBDISCS": {"param_name": "ensemble_filter_CBDISCS", "description": "Turn on or off ensemble filter CBDISCS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_HRD_PERIOD_DISTRIBUTIONS": {"param_name": "ensemble_filter_HRD_PERIOD_DISTRIBUTIONS", "description": "Turn on or off ensemble filter HRD_PERIOD_DISTRIBUTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_HRD_TIME_SLICES": {"param_name": "ensemble_filter_HRD_TIME_SLICES", "description": "Turn on or off ensemble filter HRD_TIME_SLICES. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_HRD_PERIOD_DISTRIBUTIONS_TIME_SLICES": {"param_name": "ensemble_filter_HRD_PERIOD_DISTRIBUTIONS_TIME_SLICES", "description": "Turn on or off ensemble filter HRD_PERIOD_DISTRIBUTIONS_TIME_SLICES. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_HRD_MASS_DISTRIBUTIONS": {"param_name": "ensemble_filter_HRD_MASS_DISTRIBUTIONS", "description": "Turn on or off ensemble filter HRD_MASS_DISTRIBUTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_GAIA_CMD": {"param_name": "ensemble_filter_GAIA_CMD", "description": "Turn on or off ensemble filter GAIA_CMD. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_GAIA_CMD_TIME_SLICES": {"param_name": "ensemble_filter_GAIA_CMD_TIME_SLICES", "description": "Turn on or off ensemble filter GAIA_CMD_TIME_SLICES. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_GAIA_CMD_PERIOD_DISTRIBUTIONS": {"param_name": "ensemble_filter_GAIA_CMD_PERIOD_DISTRIBUTIONS", "description": "Turn on or off ensemble filter GAIA_CMD_PERIOD_DISTRIBUTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_GAIA_CMD_PERIOD_DISTRIBUTIONS_TIME_SLICES": {"param_name": "ensemble_filter_GAIA_CMD_PERIOD_DISTRIBUTIONS_TIME_SLICES", "description": "Turn on or off ensemble filter GAIA_CMD_PERIOD_DISTRIBUTIONS_TIME_SLICES. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_GAIA_CMD_MASS_DISTRIBUTIONS": {"param_name": "ensemble_filter_GAIA_CMD_MASS_DISTRIBUTIONS", "description": "Turn on or off ensemble filter GAIA_CMD_MASS_DISTRIBUTIONS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_PULSATORS": {"param_name": "ensemble_filter_PULSATORS", "description": "Turn on or off ensemble filter PULSATORS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_TIDES": {"param_name": "ensemble_filter_TIDES", "description": "Turn on or off ensemble filter TIDES. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_PNE": {"param_name": "ensemble_filter_PNE", "description": "Turn on or off ensemble filter PNE. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_RRLYRAE": {"param_name": "ensemble_filter_RRLYRAE", "description": "Turn on or off ensemble filter RRLYRAE. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_TRANSIENTS": {"param_name": "ensemble_filter_TRANSIENTS", "description": "Turn on or off ensemble filter TRANSIENTS. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_COMENV": {"param_name": "ensemble_filter_COMENV", "description": "Turn on or off ensemble filter COMENV. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_HRD_BOKEH": {"param_name": "ensemble_filter_HRD_BOKEH", "description": "Turn on or off ensemble filter HRD_BOKEH. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_CMD_BOKEH": {"param_name": "ensemble_filter_CMD_BOKEH", "description": "Turn on or off ensemble filter CMD_BOKEH. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_IFMR": {"param_name": "ensemble_filter_IFMR", "description": "Turn on or off ensemble filter IFMR. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_RLOF": {"param_name": "ensemble_filter_RLOF", "description": "Turn on or off ensemble filter RLOF. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_BeXRB": {"param_name": "ensemble_filter_BeXRB", "description": "Turn on or off ensemble filter BeXRB. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_filter_NUMBER": {"param_name": "ensemble_filter_NUMBER", "description": "Turn on or off ensemble filter NUMBER. For a list of filters, see ensemble_macros.h.", "rest": "(null)"}, "ensemble_legacy_ensemble": {"param_name": "ensemble_legacy_ensemble", "description": "Turn on ensemble legacy population output.", "rest": "(null)"}, "legacy_yields": {"param_name": "legacy_yields", "description": "Turn on ensemble legacy yield output.", "rest": "(null)"}, "ensemble_defer": {"param_name": "ensemble_defer", "description": "Defer ensemble output.", "rest": "(null)"}, "ensemble_dt": {"param_name": "ensemble_dt", "description": "When doing ensemble calculations, data are stored and/or output every ensemble_dt Myr. See also ensemble, ensemble_logdt, ensemble_startlogtime.", "rest": "(null)"}, "ensemble_logdt": {"param_name": "ensemble_logdt", "description": "When doing ensemble calculations, and when logensembletimes is set, the ensemble is stored/output every ensemble_logdt Myr. See also ensemble, ensemble_dt, ensemble_startlogtime.", "rest": "(null)"}, "ensemble_startlogtime": {"param_name": "ensemble_startlogtime", "description": "Start log ensemble data storage/calculations/output at ensemble_startlogtime. See also ensemble, ensemble_dt, ensemble_startlogtime.", "rest": "(null)"}, "ensemble_logtimes": {"param_name": "ensemble_logtimes", "description": "When doing ensemble calculations/output, set this to act at log times rather than linear times.", "rest": "(null)"}, "postagb_legacy_logging": {"param_name": "postagb_legacy_logging", "description": "Turn on post-AGB legacy logging.", "rest": "(null)"}, "disc_legacy_logging": {"param_name": "disc_legacy_logging", "description": "Turn on disc legacy logging.", "rest": "(null)"}, "EMP_logg_maximum": {"param_name": "EMP_logg_maximum", "description": "Maximum logg that EMP stars are allowed to have. See Izzard et al 2009. See also CEMP_cfe_minimum, NEMP_nfe_minimum, EMP_minimum_age.", "rest": "(null)"}, "EMP_minimum_age": {"param_name": "EMP_minimum_age", "description": "Minimum age that EMP stars are required to have. See Izzard et al 2009. See also CEMP_cfe_minimum, NEMP_nfe_minimum, EMP_logg_maximum.", "rest": "(null)"}, "EMP_feh_maximum": {"param_name": "EMP_feh_maximum", "description": "Maximum [Fe/H] that an EMP stars may have. See Izzard et al 2009. See also CEMP_cfe_minimum, NEMP_nfe_minimum, EMP_logg_maximum, EMP_minimum_age. Default -2.0.", "rest": "(null)"}, "CEMP_cfe_minimum": {"param_name": "CEMP_cfe_minimum", "description": "Minimum [C/Fe] that CEMP stars are required to have. See Izzard et al 2009. See also NEMP_cfe_minimum, EMP_logg_maximum, EMP_minimum_age. Default 0.7.", "rest": "(null)"}, "NEMP_cfe_minimum": {"param_name": "NEMP_cfe_minimum", "description": "Minimum [N/Fe] that NEMP stars are required to have. See Izzard et al 2009, Pols et al. 2012. See also CEMP_cfe_minimum, EMP_logg_maximum, EMP_minimum_age. Default 1.0.", "rest": "(null)"}, "thick_disc_start_age": {"param_name": "thick_disc_start_age", "description": "Lookback time for the start of the thick disc star formation, e.g. 13e3 Myr. Units = Myr.", "rest": "(null)"}, "thick_disc_end_age": {"param_name": "thick_disc_end_age", "description": "Lookback time for the end of the thick disc star formation, e.g. 4e3 Myr. Units = Myr.", "rest": "(null)"}, "thick_disc_logg_min": {"param_name": "thick_disc_logg_min", "description": "Minimum logg for thick disc giants to be logged.", "rest": "(null)"}, "thick_disc_logg_max": {"param_name": "thick_disc_logg_max", "description": "Maximum logg for thick disc giants to be logged.", "rest": "(null)"}, "escape_velocity": {"param_name": "escape_velocity", "description": "A parameter used in constructing galactic chemical evolution (GCE) models. If the stellar wind velocity exceeds this value, any chemical yield from the wind is ignored, i.e. assumed lost. (km/s) Requires NUCSYN_GCE_OUTFLOW_CHECKS. Default 1e9 km/s. See also escape_fraction.", "rest": "(null)"}, "escape_fraction": {"param_name": "escape_fraction", "description": "A parameter used in constructing galactic chemical evolution (GCE) models. If the stellar wind velocity exceeds this value, any chemical yield from the wind is ignored, i.e. assumed lost. (km/s) Requires NUCSYN_GCE_OUTFLOW_CHECKS. Default 0.0. See also escape_velocity.", "rest": "(null)"}, "colour_log": {"param_name": "colour_log", "description": "If set to True, thelog is coloured with ANSI colour formatting. Requires FILE_LOG to be defined. (If clean_log is True, colours are never used.)", "rest": ""}, "log_legacy_stellar_types": {"param_name": "log_legacy_stellar_types", "description": "If set to True, we output the stellar types in the log as numbers rather than (more human-readable) letters.", "rest": ""}, "log_filename": {"param_name": "log_filename", "description": "Location of the output logging filename. If set to \"/dev/null\" then there is no logging.", "rest": ""}, "log_separator": {"param_name": "log_separator", "description": "Separator used in the standard log. By default this is an empty string.", "rest": ""}, "log_period_unit": {"param_name": "log_period_unit", "description": "Define the unit used to log orbital periods. If 'auto' or 0, the default, automatically choses the unit. ", "rest": "(null)"}, "clean_log": {"param_name": "clean_log", "description": "If TRUE, all other log formatting is ignored, arrows are off, so that the log is parseable by 3rd-party applications in a fixed form. (FALSE)", "rest": "(null)"}, "log_arrows": {"param_name": "log_arrows", "description": "Add arrows to the output log to show whether values are increasing or decreasing. (If clean_log is True, arrows are never output.)", "rest": ""}, "stopfile": {"param_name": "stopfile", "description": "File which, when it exists, will stop the current binary_c repeat run.", "rest": ""}, "stardata_dump_filename": {"param_name": "stardata_dump_filename", "description": "Location of the stardata dump file.", "rest": ""}, "stardata_load_filename": {"param_name": "stardata_load_filename", "description": "Location of the stardata file to load.", "rest": ""}, "api_log_filename_prefix": {"param_name": "api_log_filename_prefix", "description": "Location of the output logging filename prefix for the API. If set to \"/dev/null\" then there is no logging.", "rest": "0"}, "hrdiag_output": {"param_name": "hrdiag_output", "description": "Set to True to output high time-resolution Hertzstrpung-Russell diagram information. Requires HRDIAG.", "rest": "(null)"}, "internal_buffering": {"param_name": "internal_buffering", "description": "Experimental. Set to non-zero values to implement internal buffering prior to output. For use with binary_grid, you shouldn't really be playing with this.", "rest": "(null)"}, "wtts_log": {"param_name": "wtts_log", "description": "If True, enables log file output for WTTS2.", "rest": "(null)"}, "fabian_imf_log_time": {"param_name": "fabian_imf_log_time", "description": "Time at which to output for Fabian Schneider's IMF project. Requires FABIAN_IMF_LOG", "rest": "Ignore"}, "fabian_imf_log_timestep": {"param_name": "fabian_imf_log_timestep", "description": "Timestep for Fabian Schneider's IMF project logging. Requires FABIAN_IMF_LOG", "rest": "Ignore"}, "version": {"param_name": "version", "description": "Display binary_c version and build information. Also performs timing tests.", "rest": "Ignore"}, "dumpversion": {"param_name": "dumpversion", "description": "Display binary_c version number (short format).", "rest": "Ignore"}, "version_only": {"param_name": "version_only", "description": "Display binary_c version number and build information, but do not perform timing tests or anything that requires stardata to be non-NULL.", "rest": "Ignore"}, "tides_diagnosis_log": {"param_name": "tides_diagnosis_log", "description": "Enable logging to test MINT tides. Requires MINT. Choices are: 0 disabled, 1 enable lambda test.", "rest": "Ignore"}, "YBC_path": {"param_name": "YBC_path", "description": "Path to the YBC bolometric correction database (git clone https://gitlab.com/cycyustc/ybc_tables).", "rest": "0"}, "YBC_listfile": {"param_name": "YBC_listfile", "description": "File to use as YBC's .list. If omitted, this is constructed for you.", "rest": "0"}, "YBC_instruments": {"param_name": "YBC_instruments", "description": "Comma-separated list of the YBC instruments to be used when computing magnitudes, e.g. \"GAIA,SLOAN\".", "rest": "0"}, "YBC_all_instruments": {"param_name": "YBC_all_instruments", "description": "If True, we set all magnitudes associated with all known and defined instruments in the YBC library (see ybc.h for the YBC_INSTRUMENTS_LIST).", "rest": "0"}, "event_based_logging_%d": {"param_name": "event_based_logging_%d", "description": "Enable logging of event type <n> (e.g. SN, RLOF, DCO). The event logstrings will first be stored in the stardata, and at the end of the evolution they will all be printed. This deals with the evol-splitting better.", "rest": "Ignore"}, "event_based_logging_SN": {"param_name": "event_based_logging_SN", "description": "Enable logging of event type SN (e.g. SN, RLOF, DCO). The event logstrings will first be stored in the stardata, and at the end of the evolution they will all be printed. This deals with the evol-splitting better.", "rest": "Ignore"}, "event_based_logging_RLOF": {"param_name": "event_based_logging_RLOF", "description": "Enable logging of event type RLOF (e.g. SN, RLOF, DCO). The event logstrings will first be stored in the stardata, and at the end of the evolution they will all be printed. This deals with the evol-splitting better.", "rest": "Ignore"}, "event_based_logging_DCO": {"param_name": "event_based_logging_DCO", "description": "Enable logging of event type DCO (e.g. SN, RLOF, DCO). The event logstrings will first be stored in the stardata, and at the end of the evolution they will all be printed. This deals with the evol-splitting better.", "rest": "Ignore"}, "event_based_logging_GENERAL": {"param_name": "event_based_logging_GENERAL", "description": "Enable logging of event type GENERAL (e.g. SN, RLOF, DCO). The event logstrings will first be stored in the stardata, and at the end of the evolution they will all be printed. This deals with the evol-splitting better.", "rest": "Ignore"}, "david_tzo_logging": {"param_name": "david_tzo_logging", "description": "Flag to enable logging for TZO project", "rest": "Ignore"}, "david_ppisn_logging": {"param_name": "david_ppisn_logging", "description": "Flag to enable logging for PPISN project", "rest": "Ignore"}, "david_ppisn_single_logging": {"param_name": "david_ppisn_single_logging", "description": "Flag to enable logging for PPISN project capturing single star systems that underwent SN", "rest": "Ignore"}, "david_continous_rlof_logging": {"param_name": "david_continous_rlof_logging", "description": "Flag to enable the continous RLOF logging (logs every timestep that there is a RLOF)", "rest": "Ignore"}, "david_rlof_system_ensemble_logging": {"param_name": "david_rlof_system_ensemble_logging", "description": "Flag to enable the RLOF system ensemble logging (orbital properties, masses etc)", "rest": "Ignore"}, "david_ensemble_ballistic_exploration_logging": {"param_name": "david_ensemble_ballistic_exploration_logging", "description": "Flag to enable ballistic interpolation parameter ensemble logging. Used to inform the interpolation table generation.", "rest": "Ignore"}, "david_ensemble_disk_thickness_exploration_logging": {"param_name": "david_ensemble_disk_thickness_exploration_logging", "description": "Flag to enable disk thickness project ensemble logging. Used to inform the estimates of whether the accretion disk becomes thick at rcirc.", "rest": "Ignore"}, "david_log_wind_ensemble": {"param_name": "david_log_wind_ensemble", "description": "Flag to include wind outflow for single stars in ensemble. Meant for single stars really but we can expand this to binaries", "rest": "Ignore"}, "david_open_cluster_system_ensemble_logging": {"param_name": "david_open_cluster_system_ensemble_logging", "description": "Flag to enable the system ensemble logging for open clusters (orbital properties, masses etc). Requires the parameters 'open_cluster_simulation_age_myr_lower_bound', 'open_cluster_simulation_age_myr_upper_bound', 'open_cluster_simulation_mode' to be set as well.", "rest": "Ignore"}, "david_disk_photometry_ensemble_logging": {"param_name": "david_disk_photometry_ensemble_logging", "description": "Flag to calculate accretion disk interactions and occurence in the HRD and CMD. NOTE: this is under construction", "rest": "Ignore"}, "david_logging_function": {"param_name": "david_logging_function", "description": "Function to choose which kind of information gets logged Requires DAVID. Choices are: 0= None, >0 for custom logging functions", "rest": "Ignore"}, "disk_photometry_num_rings": {"param_name": "disk_photometry_num_rings", "description": "Parameter to configure the number of rings used in the disk photometry calculation. See flag DAVID_DISK_PHOTOMETRY_ENSEMBLE and setting parameter david_disk_photometry_ensemble_logging", "rest": "Ignore"}, "disk_photometry_disk_discretization_method": {"param_name": "disk_photometry_disk_discretization_method", "description": "Parameter to configure the discretization method for the ring photometry calculation. 0 = linear. 1 = logarithmic See flag DAVID_DISK_PHOTOMETRY_ENSEMBLE and setting parameter david_disk_photometry_ensemble_logging", "rest": "Ignore"}, "disk_photometry_boundary_layer_size_fraction": {"param_name": "disk_photometry_boundary_layer_size_fraction", "description": "Parameter to configure fractional boundary layer size. See flag DAVID_DISK_PHOTOMETRY_ENSEMBLE and setting parameter david_disk_photometry_ensemble_logging", "rest": "Ignore"}, "open_cluster_simulation_mode": {"param_name": "open_cluster_simulation_mode", "description": "Switch to activate the logging of the RLOF ensemble, used in combination with a given set of bounds", "rest": "Ignore"}, "open_cluster_simulation_age_myr_lower_bound": {"param_name": "open_cluster_simulation_age_myr_lower_bound", "description": "Lower bound value for the window in which we store values for the open cluster orbital property calculations. The variable open_cluster_simulatio_mode has to be set to 1. In between open_cluster_simulation_age_myr_lower_bound and open_cluster_simulation_age_myr_upper_bound we store the standard ensemble RLOF values to mimic an observation of a cluster", "rest": "Ignore"}, "open_cluster_simulation_age_myr_upper_bound": {"param_name": "open_cluster_simulation_age_myr_upper_bound", "description": "Upper bound value for the window in which we store values for the open cluster orbital property calculations. The variable open_cluster_simulatio_mode has to be set to 1. See open_cluster_simulation_age_myr_lower_bound for more info.", "rest": "Ignore"}, "open_cluster_ensemble_log10_orbital_period_binsize": {"param_name": "open_cluster_ensemble_log10_orbital_period_binsize", "description": "Binsize for log10_orbital_period for the open cluster ensemble log", "rest": "Ignore"}, "open_cluster_ensemble_orbital_eccentricity_binsize": {"param_name": "open_cluster_ensemble_orbital_eccentricity_binsize", "description": "Binsize for orbital_eccentricity for the open cluster ensemble log", "rest": "Ignore"}}}, "input": {"section_name": "input", "parameters": {"MINT_dir": {"param_name": "MINT_dir", "description": "Location of MINT algorithm data.", "rest": ""}, "MINT_load_state_file": {"param_name": "MINT_load_state_file", "description": "File from which the MINT state should be loaded.", "rest": ""}, "MINT_save_state_file": {"param_name": "MINT_save_state_file", "description": "File to which the MINT state should be saved.", "rest": ""}, "MINT_data_cleanup": {"param_name": "MINT_data_cleanup", "description": "Activate checks on incoming data to try to account for problems. Will make data-loading slower, but may fix a few things.", "rest": ""}, "MINT_MS_rejuvenation": {"param_name": "MINT_MS_rejuvenation", "description": "Turn on or off (hydrogen) main-sequence rejuvenation.", "rest": ""}, "MINT_remesh": {"param_name": "MINT_remesh", "description": "Turn on or off MINT's remeshing.", "rest": ""}, "MINT_filename_vb": {"param_name": "MINT_filename_vb", "description": "Turn on or off verbose logging of MINT filename searches. Handy for debugging when you can't get your data file to load.", "rest": ""}, "MINT_use_ZAMS_profiles": {"param_name": "MINT_use_ZAMS_profiles", "description": "Use chemical profiles at the ZAMS if MINT_use_ZAMS_profiles is TRUE, otherwise set homogeneous abundances. (Default is TRUE, so we use the profiles if they are available.)", "rest": ""}, "MINT_fallback_to_test_data": {"param_name": "MINT_fallback_to_test_data", "description": "If TRUE, use the MINT test_data directory as a fallback when data is unavailable. (FALSE)", "rest": ""}, "MINT_use_fallback_comenv": {"param_name": "MINT_use_fallback_comenv", "description": "If TRUE, use the BSE common-envelope prescription as a fallback when MINT is not available.", "rest": ""}, "MINT_disable_grid_load_warnings": {"param_name": "MINT_disable_grid_load_warnings", "description": "Use this to disable MINT's warnings when loading a grid with, e.g., missing or too much data.", "rest": ""}, "MINT_disable_warnings": {"param_name": "MINT_disable_warnings", "description": "Use this to disable all MINT's warnings.", "rest": ""}, "MINT_Kippenhahn": {"param_name": "MINT_Kippenhahn", "description": "Turn on or off MINT's Kippenhahn diagrams. If 0, off, if 1, output star 1 (index 0), if 2 output star 2 (index 1). Default 0.", "rest": ""}, "MINT_nshells": {"param_name": "MINT_nshells", "description": "Set the initial number of shells MINT uses in each star when doing nuclear burning. Note: remeshing can change this. If MINT_nshells is 0, shellular burning and other routines that require shells will not be available. (200)", "rest": ""}, "MINT_maximum_nshells": {"param_name": "MINT_maximum_nshells", "description": "Set the maximum number of shells MINT uses in each star when doing nuclear burning. Note that this will be limited to MINT_HARD_MAX_NSHELLS. (1000)", "rest": ""}, "MINT_minimum_nshells": {"param_name": "MINT_minimum_nshells", "description": "Set the minimum number of shells MINT uses in each star when doing nuclear burning. Note that this will be greater than or equal to MINT_HARD_MIN_NSHELLS, which is 0 by default. (0)", "rest": ""}, "MINT_Kippenhahn_stellar_type": {"param_name": "MINT_Kippenhahn_stellar_type", "description": "Stellar type selector for Kippenhahn plots. Set to -1 to ignore, otherwise the stellar type number for which Kippenhahn plot data should be output.", "rest": ""}, "MINT_Kippenhahn_companion_stellar_type": {"param_name": "MINT_Kippenhahn_companion_stellar_type", "description": "Companion stellar type selector for Kippenhahn plots. Set to -1 to ignore, otherwise the stellar type number for the companion for which Kippenhahn plot data should be output.", "rest": ""}, "MINT_nuclear_burning": {"param_name": "MINT_nuclear_burning", "description": "Turn on or off MINT's nuclear burning algorithm.", "rest": ""}, "MINT_minimum_shell_mass": {"param_name": "MINT_minimum_shell_mass", "description": "Minimum shell mass in MINT's nuclear burning routines.", "rest": ""}, "MINT_maximum_shell_mass": {"param_name": "MINT_maximum_shell_mass", "description": "Maximum shell mass in MINT's nuclear burning routines. :", "rest": ""}}}, "i/o": {"section_name": "i/o", "parameters": {"go": {"param_name": "go", "description": "batchmode control command", "rest": "Ignore"}, "gogo": {"param_name": "gogo", "description": "batchmode control command", "rest": "Ignore"}, "reset_stars": {"param_name": "reset_stars", "description": "Reset the star structures. Used in batchmode", "rest": "Ignore"}, "reset_stars_defaults": {"param_name": "reset_stars_defaults", "description": "Reset the star structures and set defaults. Used in batchmode", "rest": "Ignore"}, "defaults": {"param_name": "defaults", "description": "Reset all defaults. Used in batchmode", "rest": "Ignore"}, "echo": {"param_name": "echo", "description": "Activate batchmode command echoing, i.e. when you enter a command, binary_c repeats the command then executes it.", "rest": "Ignore"}, "noecho": {"param_name": "noecho", "description": "Deactivate batchmode command echoing. See 'echo'.", "rest": "Ignore"}, "noechonow": {"param_name": "noechonow", "description": "Deactivate batchmode command echoing. See 'echo'.", "rest": "Ignore"}, "bye": {"param_name": "bye", "description": "Quit binary_c. Used in batchmode.", "rest": "Ignore"}, "fin": {"param_name": "fin", "description": "batchmode control command", "rest": "Ignore"}, "reset_prefs": {"param_name": "reset_prefs", "description": "Reset preferences struct. Used in batchmode", "rest": "Ignore"}, "status": {"param_name": "status", "description": "Output batchmode status information.", "rest": "Ignore"}}}, "algorithms": {"section_name": "algorithms", "parameters": {"repeat": {"param_name": "repeat", "description": "If > 1, repeats the system as many times as required. Handy if you're using Monte-Carlo kicks and want to sample the parameter space well. Also, if you are running speed tests this is good to give a statistically more reasonable result. (See e.g. 'tbse pgo').", "rest": "(null)"}, "pause_after_repeat": {"param_name": "pause_after_repeat", "description": "If true, pauses after a repeated system is run to wait for someone to press RETURN on stdin.", "rest": "(null)"}, "random_systems": {"param_name": "random_systems", "description": "Experimental. Use this to apply random initial system parameters (masses, separations, etc.). Useful for testing only.", "rest": "(null)"}}}, "misc": {"section_name": "misc", "parameters": {"defaults_set": {"param_name": "defaults_set", "description": "Choose the set of defaults to be used by binary_c.", "rest": "(null)"}, "skip_bad_args": {"param_name": "skip_bad_args", "description": "If not set to SKIP_BAD_ARGS_NONE, skip unmatched arguments assuming they are in the form \"--x y\". Can be SKIP_BAD_ARGS_WITH_WARNING (will warn to the output buffer) or SKIP_BAD_ARGS_WITH_NO_WARNING (stays quiet). (SKIP_BAD_ARGS_NONE)", "rest": "(null)"}, "random_seed": {"param_name": "random_seed", "description": "Random number seed, usually a (possibly negative) integer. Useful for exactly reproducing the evolution of a system which involves a kick (which is a Monte-Carlo, i.e. pseudorandom, process).", "rest": "(null)"}, "random_systems_seed": {"param_name": "random_systems_seed", "description": "Random number seed for the generation of random systems. See random_systems and random_seed.", "rest": "(null)"}, "random_skip": {"param_name": "random_skip", "description": "Skip the first <random_seed> random numbers that are generated. Usually this is 0 so they are all used.", "rest": "(null)"}, "idum": {"param_name": "idum", "description": "[NB: deprecated, please use 'random_seed' instead.] Random number seed, usually a (possibly negative) integer. Useful for exactly reproducing the evolution of a system which involves a kick (which is a Monte-Carlo, i.e. pseudorandom, process).", "rest": "(null)"}, "reverse_time": {"param_name": "reverse_time", "description": "Make time go backwards. To be considered very experimental!", "rest": "(null)"}, "start_time": {"param_name": "start_time", "description": "Start time for the simulation.", "rest": "(null)"}, "warmup_cpu": {"param_name": "warmup_cpu", "description": "Uses the CPU at maximum power the given number of seconds, prior to running normal stellar evolution.", "rest": "Ignore"}, "help": {"param_name": "help", "description": "Display help pages. Usage: --help <help topic>.", "rest": "Ignore"}, "argopts": {"param_name": "argopts", "description": "Display argument options. Usage: --argopts <argument>.", "rest": "Ignore"}, "help_all": {"param_name": "help_all", "description": "Display all help pages.", "rest": "Ignore"}, "list_args": {"param_name": "list_args", "description": "Display list of arguments with their default values. Useful for batchmode.", "rest": "Ignore"}, "bjorn": {"param_name": "bjorn", "description": "Usage: --bjorn    ... shows an ASCII-art picture of Bj\u00f6rn (requires jp2a to be installed).", "rest": "0"}, "logo": {"param_name": "logo", "description": "Usage: --logo    ... shows an ASCII-art picture of the binary_c logo (requires jp2a to be installed).", "rest": "0"}, "nanchecks": {"param_name": "nanchecks", "description": "Turn nanchecks on or off. Requires SOFT_NANCHECK to be defined. True by default if so, otherwise ignored.", "rest": "(null)"}, "random_system_list": {"param_name": "random_system_list", "description": "Output a list of nrepeat random systems (see also \"repeat\") and exit.", "rest": "(null)"}}}}}, "evolution_type": "grid", "failed_count": 139, "failed_prob": 3.546197279650278e-05, "failed_systems_error_codes": [31], "errors_exceeded": false, "errors_found": true, "total_probability": 0.2971455371995682, "total_count": 492960, "start_timestamp": 1684508840.7442908, "end_timestamp": 1684540195.7518873, "time_elapsed": 31355.007596492767, "total_mass_run": 12112503.635859301, "total_probability_weighted_mass_run": 0.4889468972514483, "zero_prob_stars_skipped": 0, "date": "05/20/2023 00:49:55", "platform": "Linux-4.4.0-210-generic-x86_64-with-glibc2.23", "platform_uname": ["Linux", "astro1", "4.4.0-210-generic", "#242-Ubuntu SMP Fri Apr 16 09:57:56 UTC 2021", "x86_64", "x86_64"], "platform_machine": "x86_64", "platform_node": "astro1", "platform_release": "4.4.0-210-generic", "platform_version": "#242-Ubuntu SMP Fri Apr 16 09:57:56 UTC 2021", "platform_processor": "x86_64", "platform_python_build": "main Nov 19 2022 11:49:51", "platform_python_version": "3.9.9", "hostname": "astro1", "duration": 31355.007596492767, "CPU_time": 1505040.3646316528, "simname": "EVENTS_V2.2.4_HIGH_RES_EXPLORATION_BALLISTIC_RLOF_2021_MOE_DISTEFANO", "metallicity": 0.02}