&star_job

      show_log_description_at_start = .false.

      load_saved_model = .true.
      saved_model_name = 'solar_calibration_input.mod'
      
! The assumption is that the changes in parameters for mass, alpha, Y, Z/X, f_ov are small enough and
! that the starting model is saved early enough in the pre-main sequence period, that we can load the
! same starting model each time and make small changes to it at the start of the evolution.  The starting
! model is therefore never touched during the calibration runs.    Therefore the starting model must be
! from early pre-main sequence -- best if it is still fully convective and before nuclear burning has started.

! I believe that such early models can safely asborb fairly substantial changes in mass, alpha, Y, Z/X, f_ov
! without showing an effect on the resulting ZAMS model.  But you should check that by comparing what 
! we get by making the changes to the calibration starting model to what you would get if you started 
! fresh with a call on create pre-ms for the new parameters.   Do you find significant differences?  
! How large to the changes in parameters need to be to give a significantly different ZAMS model?  
! That would be good to know.      

      change_net = .true. ! switch nuclear reaction network
      new_net_name = 'pp_and_cno_extras.net'
	   
      set_uniform_initial_composition = .true.
	   initial_zfracs = 3 ! GS98_zfracs = 3
      initial_h1 = 0.700262d0
      initial_h2 = 0
      initial_he3 = 0.279364d-4
      initial_he4 = 0.279364d0

	   set_rate_n14pg = 'Imbriani'
	   set_rate_c12ag = 'Kunz'

      kappa_file_prefix = 'OP_gs98'
      kappa_lowT_prefix = 'lowT_fa05_gs98' ! for lower temperatures.
      
      
      change_lnPgas_flag = .true.
      new_lnPgas_flag = .true.
      

/ ! end of star_job namelist


&controls

      max_age = 4.57d9
      
      mixing_length_alpha = 2.02144520885243d0

      ! controls for output
      photostep = 50
      profile_interval = 50
      history_interval = 1
      terminal_cnt = 2
      write_header_frequency = 10


      ! atmosphere
      which_atm_option = 'photosphere_tables'
      
      ! atomic diffusion
      do_element_diffusion = .true. ! determines whether or not we do diffusion
      diffusion_dt_limit = 7d11 ! no element diffusion if dt < this limit (in seconds)
      diffusion_T_full_on = 1d3
      diffusion_T_full_off = 1d3
      
      diffusion_calculates_ionization = .true.

      diffusion_num_classes = 4 ! number of classes of species for diffusion calculations
      diffusion_class_representative(1) = 'h1'
      diffusion_class_representative(2) = 'he4'
      diffusion_class_representative(3) = 'o16'
      diffusion_class_representative(4) = 'fe56'
!   
!      ! in ascending order.  species goes into 1st class with A_max >= species A
      diffusion_class_A_max(1) = 2
      diffusion_class_A_max(2) = 4
      diffusion_class_A_max(3) = 16
      diffusion_class_A_max(4) = 10000
 
      ! timesteps
      max_years_for_timestep = 1d7           
      varcontrol_target = 1d-4

      ! mesh adjustment
      mesh_delta_coeff = 0.8
   	
   	P_function_weight = 25
   	T_function1_weight = 75
      
      xtra_coef_czb_full_on = 1
      xtra_coef_czb_full_off = 1

      xtra_coef_a_l_nb_czb = 0.45 ! above lower nonburn convective boundary
      xtra_dist_a_l_nb_czb = 20 ! above lower nonburn convective boundary

      xtra_coef_b_l_nb_czb = 0.45 ! below lower nonburn convective boundary
      xtra_dist_b_l_nb_czb = 20 ! below lower nonburn convective boundary

         
      xa_function_species(1) = 'he4'  ! name of nuclide as defined in chem_def
		xa_function_weight(1) = 130
		xa_function_param(1) = 1d-2
         
      xa_function_species(2) = 'he3'  ! name of nuclide as defined in chem_def
		xa_function_weight(2) = 60
		xa_function_param(2) = 1d-5

      ! opacity
      
      use_Type2_opacities = .false.

      cubic_interpolation_in_Z = .true.

      trace_solar_neutrinos = .false. ! if true, then output neutrino flux info

      

/ ! end of controls namelist

