'example_1Msun_solar_Z'
'example_3Msun_solar_Z'
'example_20Msun_solar_Z'
Each is a MESA work directory, which can be run or modified to replicate our results. 

Notes:

-Our models were run using a modified MESA version of r15140, which includes a fix to the neutrino losses during operator splitting mentioned in this github thread: https://github.com/MESAHub/mesa/issues/488
and corrected in: https://github.com/MESAHub/mesa/pull/496

- Our models contain a custom run_star_extras.f90 hardcoded to the size of the networks run so as to track each individual weak reaction in the network.

-An initialization bug for the low-mass models results in unrealistic, hyper-inflated values for log_Lneu_beta and log_Lneu_invbeta, when nuclear burning should be turned off entirely. This only effects the WD cooling track (08_wd_cooling_track_burning_off).

-At times (near the end of the TP-AGB) or during advanced burning in massive stars, we suppressed overshoot to get models to their final fate.

-models are run through the "run_all.com" executable.
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Output-history-data: '0p5','0p0','m0p5','m1p0','m2p0','m3p0'
contains history files for every model run, across all six metallicites:

Z = 10^0.5, 10^0, 10^-0.5, 10^-1, 10^-2, 10^-3 Zsun

Each stellar track contains the following values:

model_number log_LH log_LHe log_R log_Teff log_dt log_L log_Lneu log_Lnuc log_center_T log_center_Rho star_age center_ne20 center_c12 center_o16 center_si28 center_fe56 center_entropy center_he4 center_h1 star_mass log_Lneu_beta log_Lneu_invbeta log_Lneu_pair log_Lneu_plas log_Lneu_phot log_Lneu_brem log_Lneu_reco log_Lneu_nonnuc log_Lneu_nuc center_ye log_nps_beta log_nps_invbeta log_max_T compactness_parameter log_total_energy log_total_internal_energy log_total_radial_kinetic_energy log_total_gravitational_energy bc_U bc_B bc_V bc_R bc_I bc_J bc_H bc_K bc_L bc_Lprime bc_M abs_mag_U abs_mag_B abs_mag_V abs_mag_R abs_mag_I abs_mag_J abs_mag_H abs_mag_K abs_mag_L abs_mag_Lprime abs_mag_M lum_band_U lum_band_B lum_band_V lum_band_R lum_band_I lum_band_J lum_band_H lum_band_K lum_band_L lum_band_Lprime lum_band_M log_lum_band_U log_lum_band_B log_lum_band_V log_lum_band_R log_lum_band_I log_lum_band_J log_lum_band_H log_lum_band_K log_lum_band_L log_lum_band_Lprime log_lum_band_M avg_beta avg_invbeta he_core_mass c_core_mass


Notes:

-Some low mass models (typically higher mass 3-> 7 Msun) are terminated pre-maturely on the WD cooling track at log_L ~ -1.7 -> -3.0, due to eos issues.

-Some high mass models are halted prematurely:
8-10 Msun (near C-depletion)
10-14 Msun (late O/Ne burning, from stalled flame in a degenerate core)
M_he_core>~ 45 Msun (near He-depletion or at carbon iginition) onset of pair-instability.