star_job

Contents

star_job#

directories#

mesa_dir#

if set to the empty string, ‘’, then it defaults to using environment variable $(MESA_DIR)

mesa_dir = ''

chem_isotopes_filename#

this file is in chem_data in mesa_data_dir

chem_isotopes_filename = 'isotopes.data '

pause_before_terminate#

if true, then will pause before terminate run. this can be useful if you’d like a chance to look at the final model pgstar windows before they go away.

pause_before_terminate = .false.

cache directories#

eosDT_cache_dir#

ionization_cache_dir#

kap_cache_dir#

rates_cache_dir#

mesa uses caches to improve performance. the default location for these is in the mesa/data directory, but in some situations it is useful to keep the caches separately so, for example, multiple users can share the code and each can have a separate set of caches. ‘’ means use default location for cache.

The need for separate caches arises in cases where we need to put the main mesa directory in a location that is “read only” for a group of users (such as in a system directory that requires “root” or “superuser” to write). In that case the caches must be moved out of the main directory to locations that the user can write.

if you specify cache directories, use a separate one for each. e.g., something like this

eosDT_cache_dir = '/Users/bpaxton/mesa_caches/eosDT_cache'
ionization_cache_dir = '/Users/bpaxton/mesa_caches/ionization_cache'
kap_cache_dir = '/Users/bpaxton/mesa_caches/kap_cache'
rates_cache_dir = '/Users/bpaxton/mesa_caches/rates_cache'

If you give an empty string for the cache_dir, then if you have set the environment variable MESA_CACHES_DIR, then the cache is a subdirectory of that with one of the following names: eosDT_cache, kap_cache, ionization_cache, rates_cache if MESA_CACHES_DIR is not set or is the empty string, then the cache is a subdirectory of the corresponding data subdirectory, such as data/rates_data/cache for the rates cache.

eosDT_cache_dir = ''
ionization_cache_dir = ''
kap_cache_dir = ''
rates_cache_dir = ''

output#

echo_at_start#

echo_at_start = ''

echo_at_end#

echo_at_end = ''

show_log_description_at_start#

set this false if you want to skip the initial terminal output

show_log_description_at_start = .true.

show_net_species_info#

if true, then output a list of the species in the current net

show_net_species_info = .false.

show_net_reactions_info#

if true, then output information about the reactions in the current net

show_net_reactions_info = .false.

list_net_reactions#

if true, then output a simple list of the reactions in the current net

list_net_reactions = .false.

show_eqns_and_vars_names#

if true, then output a list of the names of the equations and variables

show_eqns_and_vars_names = .false.

pgstar_flag#

if true, activates pgplot output

pgstar_flag = .false.

disable_pgstar_during_relax_flag#

if true, disables pgplot output during relaxation operations

disable_pgstar_during_relax_flag = .true.

clear_initial_pgstar_history#

clear_pgstar_history#

clear_initial_pgstar_history = .true.
clear_pgstar_history = .false.

save_pgstar_files_when_terminate#

if true, then when the run terminates, pgstar outputs files for plots that have file_flag = .true. independently of the corresponding file_interval.

save_pgstar_files_when_terminate = .false.

history_columns_file#

if null string, use default.

history_columns_file = ''

profile_columns_file#

if null string, use default.

profile_columns_file = ''

save_model_number#

at any point during the run, you can save a model for later use

save_model_number = -111

save_model_when_terminate#

required_termination_code_string#

save final model when a run terminates only happens if satisfy required termination code if string is empty, then this matches all termination codes there can be several different alternative termination codes

save_model_when_terminate = .false.
required_termination_code_string(:) = ''

save_model_filename#

saved model root filename

save_model_filename = 'undefined'

save_photo_when_terminate#

if true, then save photo for last model before terminate the run

save_photo_when_terminate = .true.

profile_starting_model#

profile_model_number#

write profile for a specific model number

profile_starting_model = .false.
profile_model_number = -1111

show_retry_counts_when_terminate#

show_timestep_limit_counts_when_terminate#

show_retry_counts_when_terminate = .true.
show_timestep_limit_counts_when_terminate = .true.

write_profile_when_terminate#

filename_for_profile_when_terminate#

write profile to a given name upon termination

write_profile_when_terminate = .false.
filename_for_profile_when_terminate = ''

save_pulse_data_for_model_number#

save_pulse_data_when_terminate#

save_pulse_data_filename#

write pulsation data for the model (format given by s% pulse_data_format)

save_pulse_data_for_model_number = -111
save_pulse_data_when_terminate = .false.
save_pulse_data_filename = 'undefined'

report_retries#

in case you want some extra info about retries

report_retries = .false.

starting model#

By default at the start of a run a zams starting model is loaded, and then the initial_mass, initial_z, and initial_y are adjusted as necessary. However, there are alternatives. you can use a model you saved previously, or you can request the system to create a pre-main-sequence model.

BTW: the system finds the zams file by using the control called zams_filename the default zams file is for Z=0.02 and lives in data/star_data/zams_models. You can create your own zams file and use it instead – see test_suite/create_zams.

load_saved_model#

load_model_filename#

If load_saved_model is true, then use the specified model. If load_saved_model_for_RSP is true, then load the specified model and run it with RSP.

load_saved_model = .false.
load_model_filename = 'undefined'

create_pre_main_sequence_model#

If true, the code will create a starting model with uniform composition, a core temperature below 10^6 so no nuclear burning, and uniform contraction for enough luminosity to make it fully convective.

The mass is initial_mass from the controls namelist.

if initial_y is < 0 in the controls, then code uses 0.24 + 2*initial_z for initial_y.

The h1 mass fraction is set to 1 - (initial_y + initial_z). The he3 and he4 mass fractions are set according to initial_y with relative amounts set according to the AG89 solar mass fractions (from chem_def).

The metallicity is initial_z from the controls namelist with the metals fractions set according to the GS98 values (from chem_def).

to set the metals fractions, use initial_zfracs (described below)

create_pre_main_sequence_model = .false.

pre_ms_T_c#

Initial center temperature (must be below 1d6). If you have initial convergence problems creating a pre-ms model, you might try different values for pre_ms_T_c – that sometimes helps.

pre_ms_T_c = 3d5

pre_ms_guess_rho_c#

Guess for initial center density; set to 0 to let the code pick.

pre_ms_guess_rho_c = 0

pre_ms_d_log10_P#

Suggested spacing in pressure between points; set to 0 to let the code pick.

pre_ms_d_log10_P = 0

pre_ms_logT_surf_limit#

pre_ms_logP_surf_limit#

Model construction is from inside out and stops when reaches either of the following limits.

pre_ms_logT_surf_limit = 3.7d0
pre_ms_logP_surf_limit = 3.5d0

pre_ms_relax_num_steps#

Let pre-ms model settle in for this many steps before changing anything else. Make this large enough to allow L and Teff to adjust before starting history log.

pre_ms_relax_num_steps = 300

pre_ms_relax_to_start_radiative_core#

Let pre-ms model contract until just begins to have a tiny radiative core. i.e., keep going until just after stop being fully convective. This test starts after finish pre_ms_relax_num_steps.

pre_ms_relax_to_start_radiative_core = .true.

pre_ms_min_steps_before_check_radiative_core#

pre_ms_check_radiative_core_start#

pre_ms_check_radiative_core_stop#

pre_ms_check_radiative_core_Lnuc_div_L_limit#

pre_ms_check_radiative_core_min_mass#

pre_ms_relax_to_start_radiative_core. wait this many steps before start checking for radiative core pre_ms_check_radiative_core_start. only start checking after have encountered min_conv_mx1_bot < this this forces it to wait until after have become fully convective. pre_ms_check_radiative_core_stop. stop when conv_mx1_bot > this (measured in q). The relaxation to a radiative core is stopped if Lnuc/L>pre_ms_check_radiative_core_Lnuc_div_L_limit, or when the mass is below pre_ms_check_radiative_core_min_mass (in Msun).

pre_ms_min_steps_before_check_radiative_core = 50
pre_ms_check_radiative_core_start = 1d-6
pre_ms_check_radiative_core_stop = 1d-3
pre_ms_check_radiative_core_Lnuc_div_L_limit = 0.1d0
pre_ms_check_radiative_core_min_mass = 0.3d0

create_initial_model#

This is an alternative to create_pre_main_sequence_model. If true, creates an adiabatic, contracting model for given mass and radius. Assumes no nuclear burning and constant entropy. Ignores radiation pressure. Uses star controls initial_y and initial_z to set X, Y, and Z. Uses initial_zfracs to set abundances of metals.

Note: if you’d like to do-it-yourself, then you can use other_build_initial_model. In that case, in addition to setting create_initial_model, also set star controls use_other_build_initial_model. Then your run_star_extras routine will be called instead of the standard one.

create_initial_model = .false.

create_RSP_model#

create_RSP_model = .false.

radius_in_cm_for_create_initial_model#

mass_in_gm_for_create_initial_model#

Radius in cm and mass in grams.

radius_in_cm_for_create_initial_model = 0
mass_in_gm_for_create_initial_model = 0

center_logP_1st_try_for_create_initial_model#

entropy_1st_try_for_create_initial_model#

max_tries_for_create_initial_model#

abs_e01_tolerance_for_create_initial_model#

abs_e02_tolerance_for_create_initial_model#

center_logP_1st_try_for_create_initial_model = 10.9d0
entropy_1st_try_for_create_initial_model = 11.5d0
max_tries_for_create_initial_model = 100
abs_e01_tolerance_for_create_initial_model = 1d-4
abs_e02_tolerance_for_create_initial_model = 1d-4

initial_model_relax_num_steps#

Let initial model settle in for this many steps before changing anything else.

initial_model_relax_num_steps = 10

initial_model_eps#

Integration accuracy.

initial_model_eps = 0.05d0

when to stop#

steps_to_take_before_terminate#

If >= 0, stop after taking this many steps. Sets max_model_number = model_number + steps_to_take_before_terminate. Ignore if < 0.

steps_to_take_before_terminate = -1

stop_if_this_file_exists#

Every 100 steps, the code will try to open this file. If the file exists, it will terminate the run. If the file doesn’t exist, it will keep going.

stop_if_this_file_exists = 'stop_if_this_file_exists'

modifications to model#

These controls enable one to alter the MESA model at the start of a run (./rn) or after a restart (./re). Controls that only apply to the first model have ‘initial’ in their names, and are ignored for restarts.

set_initial_age#

initial_age#

if true, set initial age in years

set_initial_age = .false.
initial_age = 0

set_initial_model_number#

initial_model_number#

if true, set initial model number

set_initial_model_number = .false.
initial_model_number = 0

set_initial_number_retries#

initial_number_retries#

if true, set initial number of retries if false, number of retries set from initial model info

set_initial_number_retries = .true.
initial_number_retries = 0

set_initial_dt#

years_for_initial_dt#

seconds_for_initial_dt#

if true, set initial timestep, dt, in years

set_initial_dt = .false.
years_for_initial_dt = -1
seconds_for_initial_dt = -1

limit_initial_dt#

Like set_initial_dt, but does not increase current value for dt_next. Used in conjunction with years_for_initial_dt and seconds_for_initial_dt.

dt_next = min(dt_next, years_for_initial_dt*secyer)

limit_initial_dt = .false.

set_uniform_initial_composition#

Set uniform composition. This is useful with create_pre_main_sequence_model.

set_uniform_initial_composition = .false.

initial_h1#

initial_h2#

initial_he3#

initial_he4#

if set_uniform_initial_composition is true, then set hydrogen and helium mass fractions according to the following: If no h2 in current net, then this will be added to h1. If no he3 in current net, then this will be added to he4. When set_uniform_initial_composition = .false., defer to composition controls in star/defaults/controls.defaults.

initial_h1 = -1
initial_h2 = -1
initial_he3 = -1
initial_he4 = -1

initial_zfracs#

if set_uniform_initial_composition is true, then set metal fractions z fractions – select one of the options defined in chem/public/chem_def :

  • AG89_zfracs = 1

  • GN93_zfracs = 2

  • GS98_zfracs = 3

  • L03_zfracs = 4

  • AGS05_zfracs = 5

  • AGSS09_photospheric_zfracs = 6

  • L09_zfracs = 7

  • A09_Prz_zfracs = 8

  • MB22_photospheric_zfracs = 9

  • AAG21_photospheric_zfracs = 10 for example, initial_zfracs = 3 for GS98_zfracs or set initial_zfracs = 0 to use the special list of z fractions specified in controls (i.e., z_fraction_li, z_fraction_be, z_fraction_b, etc.)

initial_zfracs = 3

dump_missing_metals_into_heaviest#

this controls the treatment metals that are not included in the current net. if this flag is true, then the mass fractions of missing metals are added to the mass fraction of the most massive metal included in the net. if this flag is false, then the mass fractions of the metals in the net are renormalized to make up for the total mass fraction of missing metals.

dump_missing_metals_into_heaviest = .true.

file_for_uniform_xa#

set_uniform_initial_xa_from_file#

set_uniform_xa_from_file#

an alternative to the above set_uniform_initial_composition method. if set_uniform_initial_xa_from_file is .true., read list of iso name and mass fraction pairs from file file_for_uniform_xa and use them to set uniform composition. E.g., to convert the star to pure fe56, a file with just the following line will work.

fe56   1.0

file_for_uniform_xa = ''
set_uniform_initial_xa_from_file = .false.
set_uniform_xa_from_file = .false.

mix_section#

mix_initial_section#

mix_section_nzlo#

mix_section_nzhi#

fully mix section of model

mix_section = .false.
mix_initial_section = .false.
mix_section_nzlo = -1
mix_section_nzhi = -1

mix_envelope_down_to_T#

mix_initial_envelope_down_to_T#

fully mix envelope from surface down to given temperature

mix_envelope_down_to_T = 0
mix_initial_envelope_down_to_T = 0

set_abundance#

set_initial_abundance#

chem_name#

new_frac#

set_abundance_nzlo#

set_abundance_nzhi#

given a chem_name from chem_def, set its abundance to be new_frac in a given range of cells, from set_abundance_nzlo to set_abundance_nzhi

set_abundance = .false.
set_initial_abundance = .false.
chem_name = 'he3'
new_frac = 0
set_abundance_nzlo = -1
set_abundance_nzhi = -1

replace_element#

replace_initial_element#

chem_name1#

chem_name2#

replace_element_nzlo#

replace_element_nzhi#

replace one iso by another in a given range of cells chem_name1 and chem_name2 from chem_def

replace_element = .false.
replace_initial_element = .false.
chem_name1 = 'he3'
chem_name2 = 'he4'
replace_element_nzlo = -1
replace_element_nzhi = -1

relax_initial_composition#

num_steps_to_relax_composition#

relax_composition_filename#

relax composition from current to specified over number of steps. relax_composition_filename holds the desired composition profile information file format for relax composition

1st line: num_points num_species then 1 line for for each point where define desired composition xq xa(1) … xa(num_species) xq = fraction of xmstar exterior to the point where xmstar = mstar - M_center the interpolation routines require that the xq values which appear in your file must be monotonically increasing xa(i) = mass fraction of i’th species

NOTE: it is up to you to ensure that the current net isotopes match the species in the composition file. You can set show_net_species_info = .true. to check the isotopes in the net.

If timescale_for_relax_composition is negative, then the model will be adjusted such that in num_steps_to_relax_composition the desired composition is obtained. Otherwise, the abundance of each element will be updated each step as

new_xa = lambda*target_xa + (1-lambda)*current_xa

where lambda = dt/timescale_for_relax_composition. In this way, the target composition is reached when dt>=timescale_for_relax_composition.

relax_initial_composition = .false.
num_steps_to_relax_composition = 100
relax_composition_filename = ''
timescale_for_relax_composition = -1d0

relax_initial_to_xaccrete#

Like relax_initial_composition (and uses num_steps_to_relax_composition), but new composition is set by current specification of accretion abundances.

relax_initial_to_xaccrete = .false.

some modifications must be done gradually over several steps in “pseudo” evolution these operations have “relax” in their names. many have an alternative, with “set” in name, that simply make the change all at once. the “set” version is fine if star can manage to converge the modified model. but for larger changes where that’s not possible, you’ll need to “relax” instead.

relax_Y#

change_Y#

relax_initial_Y#

change_initial_Y#

relax_Y_minq#

relax_Y_maxq#

new_Y#

relax_Y = .true. gradually changes average Y, reconverging at each step. change_Y = .true. changes abundances; doesn’t reconverge the model. note: relax_dY in the controls inlist determines the rate of change

relax_Y = .false.
change_Y = .false.
relax_initial_Y = .false.
change_initial_Y = .false.
relax_Y_minq = 0d0
relax_Y_maxq = 1d0
new_Y = -1

relax_Z#

change_Z#

relax_initial_Z#

change_initial_Z#

relax_Z_minq#

relax_Z_maxq#

new_Z#

relax_Z = .true. gradually changes average Z, reconverging at each step. change_Z = .true. simply changes abundances; doesn’t reconverge the model. note: relax_dlnZ in the controls inlist determines the rate of change note: initial_zfracs are not adjusted when using these controls, except if set_uniform_initial_composition = .true., and manually setting abundances.

relax_Z = .false.
change_Z = .false.
relax_initial_Z = .false.
change_initial_Z = .false.
relax_Z_minq = 0d0
relax_Z_maxq = 1d0
new_Z = -1

relax_mass#

relax_initial_mass#

new_mass#

lg_max_abs_mdot#

Gradually change total mass by a wind to new_mass. lg_max_abs_mdot = -4 means max abs mdot 1d-4 msun/year; Set <= -100 to let code pick.

relax_mass = .false.
relax_initial_mass = .false.
new_mass = -1
lg_max_abs_mdot = -100

relax_mass_to_remove_H_env#

relax_initial_mass_to_remove_H_env#

extra_mass_retained_by_remove_H_env#

Gradually reduce total mass by a wind to remove the H envelope. Equivalent to relax_mass with new_mass = He_core_mass + extra_mass.

relax_mass_to_remove_H_env = .false.
relax_initial_mass_to_remove_H_env = .false.
extra_mass_retained_by_remove_H_env = 5d-3 ! (Msun)

relax_mass_scale#

relax_initial_mass_scale#

dlgm_per_step#

change_mass_years_for_dt#

Gradually rescale mass of star to new_mass. Rescales star mass without changing composition as function of m/mstar.

relax_mass_scale = .false.
relax_initial_mass_scale = .false.
dlgm_per_step = 1d-3
change_mass_years_for_dt = 1

relax_initial_angular_momentum#

max_steps_to_relax_angular_momentum#

timescale_for_relax_angular_momentum#

max_dt_for_relax_angular_momentum#

num_timescales_for_relax_angular_momentum#

relax_angular_momentum_filename#

relax_angular_momentum_constant_omega_center#

relax angular momentum from current to specified over a certain amount of relaxation timescales. This is done by adding an extra torque term of the form

s% extra_jdot(k) =  &
    (1d0 - exp(-s% dt/(s% job% timescale_for_relax_angular_momentum*secyer))) * &
    (desired_angular_momentum(k) - s% j_rot(k))/s% dt

and evolving the star without changing the composition for num_timescales_for_relax_angular_momentum times timescale_for_relax_angular_momentum. To circumvent convection we limit the acceleration of convective velocities using min_T_for_acceleration_limited_conv_velocity = 0 (see controls.defaults), and the timescale for relaxation should be very short (less than a second).

relax_angular_momentum_filename holds the desired angular momentum profile information file format for relax angular momentum

1st line: num_points then 1 line for for each point where define desired angular momentum xq angular_momentum xq = fraction of xmstar exterior to the point where xmstar = mstar - M_center angular_momentum = specific angular momentum in units of cm^2/s

‘relax_angular_momentum_constant_omega_center’ is used to account for points near the center that could be outside the range of the input data. In this case, normally the interpolation routine would just provide a value truncated to the edge of the data that would result in a large spike in central omega. If this option is true, then the innermost regions of the star that are outside of the range of the input data are relaxed such that their omega matches that of the innermost cell within the input data.

relax_initial_angular_momentum = .false.
max_steps_to_relax_angular_momentum = 1000
timescale_for_relax_angular_momentum = 1d-10
max_dt_for_relax_angular_momentum = 1d-9
num_timescales_for_relax_angular_momentum = 1000
relax_angular_momentum_filename = ''
relax_angular_momentum_constant_omega_center = .true.

relax_initial_entropy#

max_steps_to_relax_entropy#

timescale_for_relax_entropy#

max_dt_for_relax_entropy#

num_timescales_for_relax_entropy#

relax_entropy_filename#

get_entropy_for_relax_from_eos#

relax entropy from current to specified over a certain amount of relaxation timescales. This is done by adding an extra heating term of the form

s% extra_heat(k) =  &
    (1d0 - exp(s%lnS(k))/desired_entropy(k))*exp(s%lnE(k))/(timescale_for_relax_entropy*secyer)

and evolving the star without changing the composition for num_timescales_for_relax_entropy times timescale_for_relax_entropy. To circumvent convection we limit the acceleration of convective velocities using min_T_for_acceleration_limited_conv_velocity = 0 (see controls.defaults), and the timescale for relaxation should be very short (less than a second).

relax_entropy_filename holds the desired entropy profile information file format for relax entropy

1st line: num_points
then 1 line for for each point where define desired entropy
xq entropy
xq = fraction of xmstar exterior to the point
where xmstar = mstar - M_center
entropy = specific entropy in units of erg/gr/K

the interpolation routines require that the xq values which appear in your file must be monotonically increasing.

In case the entropy is not readily available, pairs of values of two other thermodynamic variables can be provided. The entropy is then computed using the eos module, and the composition of the stellar model (which can be set using relax_initial_composition). This is set by the option get_entropy_for_relax_from_eos which can take the values

  • ‘’: if empty, then input file directly specifies the entropy

  • ‘eosDT’: input file includes density and temperature

  • ‘eosPT’: input file includes gas pressure and temperature

  • ‘eosDE’: input file includes density and specific internal energy

when any of the eos* options is used, then each line in the input file must contain three columns instead of two, specifying the values of the two thermodynamic variables used in the order specified above. So, for example, when using ‘eosDT’ the format of the input file is

1st line: num_points
then 1 line for for each point where define desired entropy
xq density temperature
xq = fraction of xmstar exterior to the point
where xmstar = mstar - M_center
density and temperature in cgs units

relax_initial_entropy = .false.
max_steps_to_relax_entropy = 1000
timescale_for_relax_entropy = 1d-9
max_dt_for_relax_entropy = 1d-9
num_timescales_for_relax_entropy = 100
relax_entropy_filename = ''
get_entropy_for_relax_from_eos = ''

relax_dxdt_nuc_factor#

relax_initial_dxdt_nuc_factor#

new_dxdt_nuc_factor#

dxdt_nuc_factor_multiplier#

Gradually rescale dxdt_nuc_factor. At each step, multiply dxdt_nuc_factor by dxdt_nuc_factor_multiplier, until reach new_dxdt_nuc_factor.

relax_dxdt_nuc_factor = .false.
relax_initial_dxdt_nuc_factor = .false.
new_dxdt_nuc_factor = 0
dxdt_nuc_factor_multiplier = 0

relax_eps_nuc_factor#

relax_initial_eps_nuc_factor#

new_eps_nuc_factor#

eps_nuc_factor_multiplier#

Gradually rescale eps_nuc_factor. At each step, multiply eps_nuc_factor by eps_nuc_factor_multiplier until reach new_eps_nuc_factor.

relax_eps_nuc_factor = .false.
relax_initial_eps_nuc_factor = .false.
new_eps_nuc_factor = 0
eps_nuc_factor_multiplier = 0

relax_opacity_max#

relax_initial_opacity_max#

new_opacity_max#

opacity_max_multiplier#

Gradually rescale opacity_max. At each step, multiply opacity_max by opacity_max_multiplier until reach new_opacity_max.

relax_opacity_max = .false.
relax_initial_opacity_max = .false.
new_opacity_max = 0
opacity_max_multiplier = 0

relax_max_surf_dq#

relax_initial_max_surf_dq#

new_max_surf_dq#

max_surf_dq_multiplier#

Gradually rescale max_surface_cell_dq. At each step, multiply max_surface_cell_dq by opacity_max_multiplier until reach new_max_surf_dq.

relax_max_surf_dq = .false.
relax_initial_max_surf_dq = .false.
new_max_surf_dq = 0
max_surf_dq_multiplier = 0

relax_to_this_tau_factor#

dlogtau_factor#

relax_tau_factor#

relax_initial_tau_factor#

relax_tau_factor_after_core_He_burn#

relax_tau_factor_after_core_C_burn#

Must have tau_factor = 1 when atm_option = ‘table’, as surface of the model must always attach at the base of the table. However, these tau_factor settings can be used to place the surface of the model inside or outside the photosphere when atm_option = ‘T_tau’.

relax_to_this_tau_factor = 1 puts outer cell at photosphere; can go much larger or much smaller to move surface in or out from photosphere.

dlogtau_factor changes log10(tau_factor) by at most this amount per step

relax_tau_factor true gradually changes tau_factor, reconverging at each step.

relax_tau_factor_after_core_He_burn ignored if <= 0; change tau_factor when center H1 < 1e-4 and center He4 < relax_tau_factor_after_core_He_burn.

relax_tau_factor_after_core_C_burn ignored if <= 0; change tau_factor when center H1 < 1e-4, He4 < 1e-4, and center C12 < relax_tau_factor_after_core_C_burn.

relax_to_this_tau_factor = -1
dlogtau_factor = 0.1d0
relax_tau_factor = .false.
relax_initial_tau_factor = .false.
relax_tau_factor_after_core_He_burn = -1
relax_tau_factor_after_core_C_burn = -1

set_to_this_tau_factor#

set_tau_factor#

set_initial_tau_factor#

set_tau_factor_after_core_He_burn#

set_tau_factor_after_core_C_burn#

As for relax_to_this_tau_factor, but changes tau_factor without reconverging.

set_to_this_tau_factor = -1
set_tau_factor = .false.
set_initial_tau_factor = .false.
set_tau_factor_after_core_He_burn = -1
set_tau_factor_after_core_C_burn = -1

adjust_tau_factor_to_surf_density#

base_for_adjust_tau_factor_to_surf_density#

if adjust_tau_factor_to_surf_density, then at start of each step set tau_factor to current Rho(1) divided by base_for_adjust_tau_factor_to_surf_density

adjust_tau_factor_to_surf_density = .false.
base_for_adjust_tau_factor_to_surf_density = 0d0

relax_to_this_opacity_factor#

d_opacity_factor#

relax_opacity_factor#

relax_initial_opacity_factor#

relax_to_this_opacity_factor = -1
d_opacity_factor = 0.1d0
relax_opacity_factor = .false.
relax_initial_opacity_factor = .false.

relax_to_this_Tsurf_factor#

dlogTsurf_factor#

relax_Tsurf_factor#

relax_initial_Tsurf_factor#

relax_to_this_Tsurf_factor = -1
dlogTsurf_factor = 0.1d0
relax_Tsurf_factor = .false.
relax_initial_Tsurf_factor = .false.

set_to_this_Tsurf_factor#

set_Tsurf_factor#

set_initial_Tsurf_factor#

As for relax_to_this_Tsurf_factor, but changes Tsurf_factor without reconverging.

set_to_this_Tsurf_factor = -1
set_Tsurf_factor = .false.
set_initial_Tsurf_factor = .false.

relax_mass_change#

relax_initial_mass_change#

relax_mass_change_min_steps#

relax_mass_change_max_yrs_dt#

relax_mass_change_init_mdot#

relax_mass_change_final_mdot#

relax_mass_change_max_yrs_dt in years relax_mass_change_init_mdot in Msun/year

relax_mass_change = .false.
relax_initial_mass_change = .false.
relax_mass_change_min_steps = 10
relax_mass_change_max_yrs_dt = 10
relax_mass_change_init_mdot = 0
relax_mass_change_final_mdot = 0

relax_irradiation#

relax_initial_irradiation#

relax_to_this_irrad_flux#

relax_irradiation_min_steps#

relax_irradiation_max_yrs_dt#

irrad_col_depth#

extra heat near surface to model irradiation. relax_to_this_irrad_flux is flux in erg s^-1 cm^-2 from companion. we capture Pi*R^2 of that flux and distribute it uniformly in the outer 4*Pi*R^2*irrad_col_depth grams of the star, where irrad_col_depth is in g cm^-2.

relax_irradiation = .false.
relax_initial_irradiation = .false.
relax_to_this_irrad_flux = 0
relax_irradiation_min_steps = 0
relax_irradiation_max_yrs_dt = -1
irrad_col_depth = -1

set_irradiation#

set_initial_irradiation#

set_to_this_irrad_flux#

as for relax_irradiation but sets values and does not reconverge

set_irradiation = .false.
set_initial_irradiation = .false.
set_to_this_irrad_flux = 0

change_RTI_flag#

change_initial_RTI_flag#

new_RTI_flag#

RTI variables RTI_flag is true if we are doing Rayleigh-Taylor Instabilities

change_RTI_flag = .false.
change_initial_RTI_flag = .false.
new_RTI_flag = .false.

change_RSP_flag#

change_initial_RSP_flag#

new_RSP_flag#

RSP variables RSP_flag is true if we are doing radial stellar pulsations

change_RSP_flag = .false.
change_initial_RSP_flag = .false.
new_RSP_flag = .false.

velocity variables#

change_v_flag#

change_initial_v_flag#

new_v_flag#

change whether MESA evolves a (radial) velocity variable, v, defined at cell boundaries

change_v_flag = .false.
change_initial_v_flag = .false.
new_v_flag = .false.

center_ye_limit_for_v_flag#

automatically turn on velocities if center_ye drops below this limit. this is useful for evolution leading up to core collapse.

center_ye_limit_for_v_flag = 0.45d0

change_u_flag#

change_initial_u_flag#

new_u_flag#

change whether MESA evolves a (radial) velocity variable, u, defined at cell centers. this is an alternative to v at cell boundaries. can use one or the other, but not both.

change_u_flag = .false.
change_initial_u_flag = .false.
new_u_flag = .false.

change_reconstruction_flag#

change_initial_reconstruction_flag#

new_reconstruction_flag#

change whether MESA reconstruction variables with Riemann. only applies when u_flag is true.

change_reconstruction_flag = .false.
change_initial_reconstruction_flag = .false.
new_reconstruction_flag = .false.

rotation controls#

new_rotation_flag#

change_rotation_flag#

change_initial_rotation_flag#

rotation is enabled only if rotation_flag is true new_rotation_flag is only used if change_rotation_flag is true if change_rotation_flag true, then change rotation_flag to new_rotation_flag

NOTE: why 2 flags? because I want 3 options: set true, set false, and leave it alone. there are of course other ways to get 3 options, but this is what we have.

new_rotation_flag = .false.
change_rotation_flag = .false.
change_initial_rotation_flag = .false.

the following only apply when rotation is already on (i.e., when rotation_flag is true), including when you have just done change_rotation_flag true. all of these initialize the model to uniform omega (i.e. “solid body”)

new_omega#

set_omega#

set_initial_omega#

new_omega in rad/sec set_omega applies when do ./rn or ./re; if true, sets uniform omega = new_omega set_initial_omega only applies at start of run, not for restarts if true, sets uniform omega = new_omega

new_omega = 0
set_omega = .false.
set_initial_omega = .false.

new_omega_div_omega_crit#

set_omega_div_omega_crit#

set_initial_omega_div_omega_crit#

as above, but sets omega/omega_crit omega_crit is defined as:

gamma_factor = 1d0 - min(L_div_Ledd, 0.9999d0)
omega_crit = sqrt(gamma_factor*s% cgrav(k)*s% m_grav(k)/pow3(s% r(k)))

new_omega_div_omega_crit = 0
set_omega_div_omega_crit = .false.
set_initial_omega_div_omega_crit = .false.

new_surface_rotation_v = 0 ! (km sec^1)#

set_surface_rotation_v = .false.#

set_initial_surface_rotation_v = .false.#

as above, but sets surface velocity in km/sec

new_surface_rotation_v = 0
set_surface_rotation_v = .false.
set_initial_surface_rotation_v = .false.

the previous controls are “one shot” – they set omega once and are done. however you might need to set omega for several models in a row in order to give things a chance to adjust to the change. the following controls let you do that.

set_omega_step_limit#

if model_number is <= this, then do set_omega

set_omega_step_limit = -1

set_omega_div_omega_crit_step_limit#

if model_number is <= this, then do set_omega_div_omega_crit

set_omega_div_omega_crit_step_limit = -1

set_surf_rotation_v_step_limit#

if model_number is <= this, then do set_surface_rotation_v

set_surf_rotation_v_step_limit = -1

set_near_zams_omega_steps#

set_near_zams_omega_div_omega_crit_steps#

set_near_zams_surface_rotation_v_steps#

You might want to start a run at pre-ms but only turn on rotation when near zams rather than force you to stop the run near zams, change the inlist, and restart. The following will turn on rotation automatically. The working definition of “near zams” is L_nuc_burn_total/L_phot >= Lnuc_div_L_zams_limit Lnuc_div_L_zams_limit is in the controls part of the inlist.

The following apply when rotation is off and model satisfies the “near zams” test. Each turns on rotation and sets a step limit

only applies if > 0

set_omega_step_limit = model_number + set_near_zams_omega_steps - 1

set_near_zams_omega_steps = -1

only applies if > 0

set_omega_div_omega_crit_step_limit =
    model_number + set_near_zams_omega_div_omega_crit_steps - 1

set_near_zams_omega_div_omega_crit_steps = -1

only applies if > 0

set_surf_rotation_v_step_limit =  model_number + set_surf_rotation_v_step_limit - 1

set_near_zams_surface_rotation_v_steps = -1

num_steps_to_relax_rotation#

use num_steps_to_relax_rotation steps to relax omega to new value

num_steps_to_relax_rotation = 100

relax_omega_max_yrs_dt#

relax_omega_max_yrs_dt sets a maximum time step used during the relaxation process < 0 implies MESA chooses the step. Useful number is 1d4 if num_steps_to_relax_rotation > ~150

relax_omega_max_yrs_dt = 1d9

relax_omega#

relax_initial_omega#

near_zams_relax_omega#

if relax_omega true, relax to value of new_omega. applies when do ./rn or ./re relax_initial_omega only applies at start of run, not for restarts. near_zams_relax omega applies when “near zams”. The working definition of “near zams” is L_nuc_burn_total/L_phot >= Lnuc_div_L_zams_limit Lnuc_div_L_zams_limit is in the controls part of the inlist.

relax_omega = .false.
relax_initial_omega = .false.
near_zams_relax_omega = .false.

relax_omega_div_omega_crit#

relax_initial_omega_div_omega_crit#

near_zams_relax_omega_div_omega_crit#

as above for relax_omega, but for omega/omega_crit

relax_omega_div_omega_crit = .false.
relax_initial_omega_div_omega_crit = .false.
near_zams_relax_omega_div_omega_crit = .false.

relax_surface_rotation_v#

relax_initial_surface_rotation_v#

near_zams_relax_initial_surface_rotation_v#

as above for relax_omega, but for surface speed

relax_surface_rotation_v = .false.
relax_initial_surface_rotation_v = .false.
near_zams_relax_initial_surface_rotation_v = .false.

new_D_omega_flag#

change_D_omega_flag#

change_initial_D_omega_flag#

new_D_omega_flag = .false.
change_D_omega_flag = .false.
change_initial_D_omega_flag = .false.

new_am_nu_rot_flag#

change_am_nu_rot_flag#

change_initial_am_nu_rot_flag#

use_D_omega_for_am_nu_rot#

if am_nu_rot_flag is true, use time and space smoothed am_nu_rot like D_omega else if D_omega_flag and use_D_omega_for_am_nu_rot, use D_omega for am_nu_rot else use am_nu_rot from current model with no smoothing

new_am_nu_rot_flag = .false.
change_am_nu_rot_flag = .false.
change_initial_am_nu_rot_flag = .false.
use_D_omega_for_am_nu_rot = .true.

relax_core#

relax_initial_core#

new_core_mass#

dlg_core_mass_per_step#

relax_core_years_for_dt#

core_avg_rho#

core_avg_eps#

controls for nonzero center M (mass), R (radius), L (luminosity) (e.g., to model neutron star envelope or rocky core planet) new_core_mass in Msun units. If you have convergence problems, you’ll need to reduce the mass/step dlg_core_mass_per_step and timestep relax_core_years_for_dt values. core_avg_rho in g/cm^3 and core_avg_eps in ergs/g/sec are just examples. Adjust them to values appropriate for your application.

relax_core = .false.
relax_initial_core = .false.
new_core_mass = 0
dlg_core_mass_per_step = 1d-3
relax_core_years_for_dt = 1
core_avg_rho = 10
core_avg_eps = 1d-6

relax_M_center#

relax_initial_M_center#

relax_M_center_dt#

Like relax_mass_scale, but all change in mass goes into M_center. NOTE: new_mass is new total mass for star, not the new M_center value. uses dlgm_per_step in same way as relax_mass_scale. relax_M_center_dt in seconds

Example: If you want to end up with total mass = 1.4 and M_center = 1.3, start with star_mass = total - center = 0.1 = mass exterior to center. Then relax_M_center with new_mass = 1.4. That will give a new total mass of 1.4 by changing M_center. The mass exterior to the center will stay = 0.1, so the final M_center will be 1.3.

relax_M_center = .false.
relax_initial_M_center = .false.
relax_M_center_dt = 3.1558149984d1

relax_R_center#

relax_initial_R_center#

new_R_center#

dlgR_per_step#

relax_R_center_dt#

as above for the mass, but for the radius. new_R_center in cm. relax_R_center_dt in seconds.

relax_R_center = .false.
relax_initial_R_center = .false.
new_R_center = 0
dlgR_per_step = 3d-3
relax_R_center_dt = 3.1558149984d1

zero_alpha_RTI#

zero_initial_alpha_RTI#

zero_alpha_RTI = .false.
zero_initial_alpha_RTI = .false.

set_v_center#

set_initial_v_center#

set_v_center = .false.
set_initial_v_center = .false.

relax_v_center#

relax_initial_v_center#

new_v_center#

dv_per_step#

relax_v_center_dt#

new_v_center in cm/s. relax_v_center_dt in seconds.

relax_v_center = .false.
relax_initial_v_center = .false.
new_v_center = 0
dv_per_step = 0
relax_v_center_dt = 0

set_L_center#

set_initial_L_center#

set_L_center = .false.
set_initial_L_center = .false.

relax_L_center#

relax_initial_L_center#

new_L_center#

dlgL_per_step#

relax_L_center_dt#

as above for the mass, but for the luminosity. new_L_center in erg/s. relax_L_center_dt in seconds.

relax_L_center = .false.
relax_initial_L_center = .false.
new_L_center = 0
dlgL_per_step = 5d-2
relax_L_center_dt = 3.1558149984d1

remove_initial_center_at_cell_k#

remove_initial_center_by_temperature#

remove_initial_center_by_mass_fraction_q#

remove_initial_center_by_delta_mass_gm#

remove_initial_center_by_delta_mass_msun#

remove_initial_center_by_mass_gm#

remove_initial_center_by_mass_msun#

remove_initial_center_by_radius_cm#

remove_initial_center_by_radius_Rsun#

remove_initial_center_by_he4#

remove_initial_center_by_c12_o16#

remove_initial_center_by_si28#

remove_initial_center_to_reduce_co56_ni56#

remove_initial_center_by_ye#

remove_initial_center_by_entropy#

remove_initial_center_by_infall_kms#

allows the core to be removed. ignored if <= 0 value for si28 is mass fraction at which to make mass cut i.e. cut at first location going inward where mass fraction of si28 >= this limit value for ye is electron per baryon number for cut value for infall_kms is infall speed in km per sec to make the cut

remove_initial_center_at_cell_k = 0
remove_initial_center_by_temperature = 0
remove_initial_center_by_mass_fraction_q = 0
remove_initial_center_by_delta_mass_gm = 0
remove_initial_center_by_delta_mass_Msun = 0
remove_initial_center_by_mass_gm = 0
remove_initial_center_by_mass_Msun = 0
remove_initial_center_by_radius_cm = 0
remove_initial_center_by_radius_Rsun = 0
remove_initial_center_by_he4 = 0
remove_initial_center_by_c12_o16 = 0
remove_initial_center_by_si28 = 0
remove_initial_center_to_reduce_co56_ni56 = 0
remove_initial_center_by_ye = 0
remove_initial_center_by_entropy = 0
remove_initial_center_by_infall_kms = 0

remove_center_at_cell_k#

remove_center_by_temperature#

remove_center_by_mass_fraction_q#

remove_center_by_delta_mass_gm#

remove_center_by_delta_mass_Msun#

remove_center_by_mass_gm#

remove_center_by_mass_Msun#

remove_center_by_radius_cm#

remove_center_by_radius_Rsun#

remove_center_by_he4#

remove_center_by_c12_o16#

remove_center_by_si28#

remove_center_to_reduce_co56_ni56#

remove_center_by_ye#

remove_center_by_entropy#

remove_center_by_infall_kms#

allows the core to be removed. ignored if <= 0

remove_center_at_cell_k = 0
remove_center_by_temperature = 0
remove_center_by_mass_fraction_q = 0
remove_center_by_delta_mass_gm = 0
remove_center_by_delta_mass_Msun = 0
remove_center_by_mass_gm = 0
remove_center_by_mass_Msun = 0
remove_center_by_radius_cm = 0
remove_center_by_radius_Rsun = 0
remove_center_by_he4 = 0
remove_center_by_c12_o16 = 0
remove_center_by_si28 = 0
remove_center_to_reduce_co56_ni56 = 0
remove_center_by_ye = 0
remove_center_by_entropy = 0
remove_center_by_infall_kms = 0

remove_initial_fe_core#

remove_fe_core#

remove_initial_fe_core = .false.
remove_fe_core = .false.

remove_initial_center_at_inner_max_abs_v#

remove_center_at_inner_max_abs_v#

remove_center_set_zero_v_center#

remove_initial_center_at_inner_max_abs_v = .false.
remove_center_at_inner_max_abs_v = .false.
remove_center_set_zero_v_center = .false.

remove_fallback_at_each_step#

fallback_check_total_energy#

remove_fallback_speed_limit#

if fallback_check_total_energy is false, starting at innermost cell, remove the region of cells that all have infall speed greater than remove_fallback_speed_limit in units of sound speed.

if fallback_check_total_energy is true, integrate total energy outward from innermost cell. if integral goes negative, then have bound inner region. continue outward until reach a cell that has local pe+ke+ie > 0. delete everything inward of that cell.

remove_fallback_at_each_step = .false.
fallback_check_total_energy = .false.
remove_fallback_speed_limit = 0.1d0

remove_center_adjust_L_center#

remove_center_adjust_L_center = .true.

limit_center_logP_at_each_step#

at start of each step remove center cells if necessary to keep logP at innermost cell >= this limit.

limit_center_logP_at_each_step = -1d99

zero_initial_inner_v_by_mass_msun#

zero_inner_v_by_mass_Msun#

zero_initial_inner_v_by_mass_Msun = 0
zero_inner_v_by_mass_Msun = 0

remove_center_logRho_limit#

remove_center_logRho_limit = -1d99

remove_initial_surface_at_cell_k#

remove_initial_surface_at_he_core_boundary#

remove_initial_surface_by_optical_depth#

remove_initial_surface_by_density#

remove_initial_surface_by_pressure#

remove_initial_surface_by_mass_fraction_q#

remove_initial_surface_by_mass_gm#

remove_initial_surface_by_mass_msun#

remove_initial_surface_by_radius_cm#

remove_initial_surface_by_radius_Rsun#

remove_initial_surface_by_v_surf_km_s#

remove_initial_surface_by_v_surf_div_cs#

remove_initial_surface_by_v_surf_div_v_escape#

allows the outer envelope to be removed. ignored if <= 0

remove_initial_surface_at_cell_k = 0
remove_initial_surface_at_he_core_boundary = 0
remove_initial_surface_by_optical_depth = 0
remove_initial_surface_by_density = 0
remove_initial_surface_by_pressure = 0
remove_initial_surface_by_mass_fraction_q = 0
remove_initial_surface_by_mass_gm = 0
remove_initial_surface_by_mass_Msun = 0
remove_initial_surface_by_radius_cm = 0
remove_initial_surface_by_radius_Rsun = 0
remove_initial_surface_by_v_surf_km_s = 0
remove_initial_surface_by_v_surf_div_cs = 0
remove_initial_surface_by_v_surf_div_v_escape = 0

remove_surface_at_cell_k#

remove_surface_at_he_core_boundary#

remove_surface_by_optical_depth#

remove_surface_by_density#

remove_surface_by_pressure#

remove_surface_by_mass_fraction_q#

remove_surface_by_mass_gm#

remove_surface_by_mass_Msun#

remove_surface_by_radius_cm#

remove_surface_by_radius_Rsun#

remove_surface_by_v_surf_km_s#

remove_surface_by_v_surf_div_cs#

remove_surface_by_v_surf_div_v_escape#

min_q_for_remove_surface_by_v_surf_div_v_escape#

max_q_for_remove_surface_by_v_surf_div_v_escape#

allows the outer envelope to be removed. ignored if <= 0

remove_surface_at_cell_k = 0
remove_surface_at_he_core_boundary = 0
remove_surface_by_optical_depth = 0
remove_surface_by_density = 0
remove_surface_by_pressure = 0
remove_surface_by_mass_fraction_q = 0
remove_surface_by_mass_gm = 0
remove_surface_by_mass_Msun = 0
remove_surface_by_radius_cm = 0
remove_surface_by_radius_Rsun = 0
remove_surface_by_v_surf_km_s = 0
remove_surface_by_v_surf_div_cs = 0
remove_surface_by_v_surf_div_v_escape = 0
min_q_for_remove_surface_by_v_surf_div_v_escape = 0d0
max_q_for_remove_surface_by_v_surf_div_v_escape = 1d0

report_mass_not_fe56#

reports mass that is not fe56

report_mass_not_fe56 = .false.

report_cell_for_xm#

in grams. if > 0 then write smallest k s.t. mass in cells 1 to k is >= report_cell_for_xm

report_cell_for_xm = -1

set_to_xa_for_accretion#

set_initial_to_xa_for_accretion#

set_nzlo#

set_nzhi#

changes the composition to the mass fractions xa_for_accretion. useful for creating a model with specific uniform composition. set_to_xa_for_accretion true, means do when start or restart. set_initial_to_xa_for_accretion true, means do for start but not for restarts. nzlo and nzhi determine the range of cells that will be changed. nzlo < 0 means change out to surface. nzhi < 0 or nzhi > number of cells means change to center.

set_to_xa_for_accretion = .false.
set_initial_to_xa_for_accretion = .false.
set_nzlo = -1
set_nzhi = -1

set_initial_cumulative_energy_error#

set_cumulative_energy_error#

set_cumulative_energy_error_at_step#

set_cumulative_energy_error_each_relax#

set_initial_cumulative_energy_error is done when execute rn script set_cumulative_energy_error is done when execute rn script or re script set_cumulative_energy_error_at_step is done before the specified step in all cases, the value is set to new_cumulative_energy_error

set_initial_cumulative_energy_error = .false.
set_cumulative_energy_error = .false.
set_cumulative_energy_error_at_step = -1
set_cumulative_energy_error_each_step_if_age_less_than = -1d99
set_cumulative_energy_error_each_relax = .true.
new_cumulative_energy_error = 0d0

nuclear reactions#

change_net#

new_net_name#

change_initial_net#

For switching reaction networks. new_net_name only used if change_net if true. The list of network names can be found in $MESA_DIR/data/net_data/nets.

change_net = .false.
new_net_name = ''
change_initial_net = .false.

adjust_abundances_for_new_isos#

If false, new isos initial abundance set to 0.

adjust_abundances_for_new_isos = .true.

Users can also provide tabulated rates for any of the reactions. Tabulated rates automatically take priority over any other options for the reaction. e.g., if you provide a rate table for c12ag, those rates will be used

To provide tabulated rates: create a file of (T8, rate) pairs as in data/rates_data/rate_tables You can give as many pairs as you want with any spacing in T8. The first uncommented line of the file should be a number giving the total number of (T8, rate) pairs in the subsequent lines. The following lines are your specified values of T8 and rate separated by a single space, one pair per line. Add the filename to rate_list.txt along with the name of the rate you want it to govern, either in data/rates_data/rate_tables or in a local directory specified with the rate_tables_dir control. Be aware that if you choose to put the modified rate_list.txt in data/rates_data/rate_tables rather than a local directory, your custom tabulated rate will override the rate for that reaction for all future MESA runs.

If the reaction you wish to control does not already have a name that MESA will recognize, you will also need to add it to the file specified by net_reaction_filename (defaults to reactions.list). The default version of this file is located in data/rates_data. If you place a modified copy of this file in your work directory, it will take precedence.

num_special_rate_factors#

reaction_for_special_factor#

special_rate_factor#

filename_of_special_rate#

For using other special rate factors. num_special_rate_factors must be <= max_num_special_rate_factors.

num_special_rate_factors = 0
reaction_for_special_factor(:) = ''
special_rate_factor(:) = 1

If set, we read this filename from the local work directory, then try data/rates_data/rate_tables. This enables using the MESA provide custom rate tables with out changing the default for everyone. Note we still multiple the loaded rate by special_rate_factor so leave that as 1 if you want the rate to be unchanged.

For instance setting:

num_special_rate_factors = 1 reaction_for_special_factor(1) = ‘r_c12_ag_o16’ special_rate_factor(1) = 1 filename_of_special_rate(1) = ‘r_c12_ag_o16_kunz.txt’

Recovers the old set_rate_c12ag = ‘Kunz’ option

filename_of_special_rate(:) = ‘’

use_3a_fl87#

If true then the triple alpha reaction is taken from Fushiki and Lamb, Apj, 317, 368-388, 1987 This replaces the old set_rate_3a = ‘Fl87’ option

use_3a_fl87 = .false.

auto_extend_net#

h_he_net#

co_net#

adv_net#

If auto_extend_net true, then automatically extend the net as needed from h_he_net to co_net and then to adv_net.

auto_extend_net = .true.
h_he_net = 'basic.net'
co_net = 'co_burn.net'
adv_net = 'approx21.net'

enable_adaptive_network#

min_x_for_keep#

min_x_for_n#

min_x_for_add#

max_Z_for_add#

max_N_for_add#

max_A_for_add#

Heger-style adaptive network (Woosley, Heger, et al, ApJSS, 151:75-102, 2004). If enable_adaptive_network is true, then at each step, the system calculates a new set of isos according to the following rules:

for each iso in the current net:
let Z = number of protons in the iso and N = number of neutrons.
let x = max mass fraction for the iso in any cell in the model.
if x >= min_x_for_keep then include the iso in new net.
if x >= min_x_for_n then include following related isos:
(Z,N+1) (Z,N-1) – add or remove neutron
if x >= min_x_for_add then include following related isos:
(Z+1,N) (Z-1,N) – add or remove proton
(Z+2,N+2) (Z-2,N-2) – add or remove alpha
(Z+2,N+1) (Z-2,N-1) – exchange neutron/alpha
(Z+1,N+2) (Z-1,N-2) – exchange proton/alpha
(Z+1,N-1) (Z-1,N+1) – exchange proton/neutron
(Z+4,N+4) (Z+3,N+4) – extend alpha chain

Isos in the previous net can be dropped if they have x < min_x_for_keep and no other iso in the previous net causes them to be included in the new net. The new net has the included isos and all relevant reactions. The definition for the new net is saved to a text file in your local “nets” directory. The file name is composed of the model number and the number of species.

enable_adaptive_network = .false.
min_x_for_keep = 1d-5
min_x_for_n = 1d-4
min_x_for_add = 1d-4
max_Z_for_add = 999
max_N_for_add = 999
max_A_for_add = 999

net_reaction_filename#

Looks first in current directory, then in mesa_data_dir/rates_data.

net_reaction_filename = 'reactions.list'

jina_reaclib_filename#

Empty string means use current standard version. Which is defined in rates/public/rates_def.f90 as reaclib_filename and is currently ‘jina_reaclib_results_20171020_default’

Else give name of file in directory mesa/data/rates_data, e.g., jina_reaclib_results_20130213default2 (which is an 18.8 MB file of rates data). To use previous version, set to jina_reaclib_results_v2.2.

If you change reaclib version, you should clear the cache after making the change in order to ensure that cached rates from the default reaclib version are not being read. (You can use the script empty_caches in $MESA_DIR.)

In order to avoid this caching issue, one can also specify a local rates cache directory via the control rates_cache_dir.

jina_reaclib_filename = ''

jina_reaclib_min_T9#

set jina reaclib rates to zero for T9 <= this. if this control is <= 0, then use the standard default from rates. need <= 3d-3 for pre-ms li7 burning if change this, must remove old cached rates from data/rates_data/cache

jina_reaclib_min_T9 = -1

rate_tables_dir#

When MESA looks for the files rate_list.txt and weak_rate_list.txt, it will look in a local directory with this name first. If doesn’t find one, it will use the one in data/rates_data/rate_tables.

rate_tables_dir = 'rate_tables'

rate_cache_suffix#

If this not empty, then use it when creating names for cache files for reaction rates from rate_tables_dir. If empty, the suffix will be ‘0’.

rate_cache_suffix = ''

T9_weaklib_full_off#

T9_weaklib_full_on#

Weak rates blend weaklib and reaclib according to temperature. These can be used to overwrite the defaults in mesa/rates/public/rates_def

  • T9_weaklib_full_off : use pure reaclib for T <= this (ignore if <= 0)

  • T9_weaklib_full_on : use pure weaklib for T >= this (ignore if <= 0)

T9_weaklib_full_off = 0.01d0
T9_weaklib_full_on = 0.02d0

weaklib_blend_hi_Z#

Ignore if <= 0. Blend for intermediate temperatures. For high Z elements, switch to reaclib at temp where no longer fully ionized. As rough approximation for this, we switch at Fe to higher values of T9.

weaklib_blend_hi_Z = 26

T9_weaklib_full_off_hi_Z#

T9_weaklib_full_on_hi_Z#

If input element has Z >= weaklib_blend_hi_Z, then use the following T9 limits:

  • T9_weaklib_full_off_hi_Z : use pure reaclib for T <= this (ignore if <= 0)

  • T9_weaklib_full_on_hi_Z : use pure weaklib for T >= this (ignore if <= 0)

T9_weaklib_full_off_hi_Z = 0.063d0
T9_weaklib_full_on_hi_Z = 0.073d0

use small net for solver iterations only#

change_small_net#

new_small_net_name#

change_initial_small_net#

For switching reaction networks for use as small net in solver iterations. small net is only used when also doing split mixing. if small_net_name is empty string, then solver uses the standard net rather than the small one. new_small_net_name only used if change_small_net if true.

change_small_net = .false.
new_small_net_name = ''
change_initial_small_net = .false.

controls for other weak rate sources#

use_suzuki_weak_rates#

If this is true, use the A=17-28 weak reaction rates from

Suzuki, Toki, and Nomoto (2016) Electron-capture and $beta$-decay rates for sd-shell nuclei in stellar environments relevant to high-density O-Ne-Mg cores http://adsabs.harvard.edu/abs/2016ApJ…817..163S

If you make use of these rates, please cite the above paper.

use_suzuki_weak_rates = .false.

use_special_weak_rates#

If this is true, calculate special weak rates using the approach described in Section 8 of Paxton et al. (2015).

use_special_weak_rates = .false.

special_weak_states_file#

File specifying which states to include

Provide the low-lying energy levels of a given nucleus. These are needed to calculate the partition function and to indicate which states have allowed transitions. Each isotope should have an entry of the form

<name> <nlevels>
<E_1> <J_1>
...
<E_n> <J_n>

where E = energy, J = spin.

special_weak_states_file = 'special_weak_rates.states'

special_weak_transitions_file#

File specifying to include

These are the transitions for electron capture / beta decay reactions that should be used.

Each reaction should have and entry of the form

<iso1> <iso2> <ntrans>
<si_1> <sf_1> <logft_1>
...
<si_n> <sf_n> <logft_n>

where si / sf are the n-th parent / daughter state, counting in the order that you specified in the states file. logft is the comparative half-life of that transition.

special_weak_transitions_file = 'special_weak_rates.transitions'

ion_coulomb_corrections#

select which expression for the ion chemical potential to use to calculate the energy shift associated with changing ion charge

  • ‘none’: no corrections

  • ‘DGC1973’: Dewitt, Graboske, & Cooper, M. S. 1973, ApJ, 181, 439

  • ‘I1993’: Ichimaru, 1993, Reviews of Modern Physics, 65, 255

  • ‘PCR2009’: Potekhin, Chabrier, & Rogers, 2009, Phys. Rev. E, 79, 016411

ion_coulomb_corrections = 'none'

electron_coulomb_corrections#

select which expression to use to calculate the shift in the electron chemical potential at the location of the nucleus

  • ‘none’: no corrections

  • ‘ThomasFermi’: Thomas-Fermi theory

  • ‘Itoh2002’: Itoh et al., 2002, ApJ, 579, 380

electron_coulomb_corrections = 'none'

ionization controls#

ionization_file_prefix#

ionization_Z1_suffix#

Prefix and suffix of ionization files.

ionization_file_prefix = 'ion'
ionization_Z1_suffix = ''

“extra” parameters#

For use by your run_star_extras routines.

extras_lipar#

extras_ipar#

extras_lipar number of integer parameters in extras_ipar. Must be <= max_extras_params (defined in run_star_support)

extras_lipar = 0
extras_ipar(:) = 0

extras_lrpar#

extras_rpar#

extras_lrpar number of real(dp) parameters in extras_rpar. Must be <= max_extras_params (defined in run_star_support)

extras_lrpar = 0
extras_rpar(:) = 0d0

extras_lcpar#

extras_cpar#

extras_lcpar number of string parameters in extras_cpar. Must be <= max_extras_params (defined in run_star_support).

extras_lcpar = 0
extras_cpar(:) = ''

extras_llpar#

extras_lpar#

extras_llpar number of logical parameters in extras_lpar. Must be <= max_extras_params (defined in run_star_support).

extras_llpar = 0
extras_lpar(:) = .false.

Color Files#

color_num_files#

color_file_names#

color_num_colors#

Filenames for each bolometric correction (BC) table to load Must set the number of files to load Must be <= max_num_color_files (defined in colors_def.f90). Must set the number of BC’s in each file (May be different for each file). Must be <= max_num_bcs_per_file (defined in colors_def.f90). Files should be structured as: Teff log_g M_div_h filter1 filter2 …. where filter1 is the name of the filter (No spaces allowed in name) Names must be unique across all files loaded and are case sensitive. For a filter named filter1 history output will be bc_filter1 for bolometric corrections and abs_mag_filter1 for absolute magnitude

Do not name any column with square brackets ([]) for instance [Fe/H] as this breaks the code

color_num_files = -1
color_file_names(:) = ''
color_num_colors(:) = -1

Default file from Lejeune, Cuisinier, Buser (1998) A&AS 130, 65-75 Can be replaced if need be. The filter names are U B V R I J H K L Lprime M (case sensitive)

color_num_files = 1
color_file_names(1) = 'lcb98cor.dat'
color_num_colors(1) = 11

Set of blackbody bolometric corrections in UBVRI Can be used at the same time as the lcb98cor.dat file Filter names bb_U bb_b bb_V bb_R bb_I color_num_files=2 color_file_names(2)=’blackbody_johnson.dat’ color_num_colors(2)=5

misc#

first_model_for_timing#

steps_before_start_timing#

To get a breakdown of where the time is going set first_model_for_timing to determine when the clocks start. At the end of the run, there will be some output to the terminal showing times.

first_model_for_timing = -1
steps_before_start_timing = -1

set_max_dt_to_frac_lifetime#

max_frac_of_lifetime_per_step#

limit max timestep. If true, set max_timestep and max_years_for_timestep according to expected lifetime as a function of mass. Use the Iben & Laughlin (1989) formula to estimate lifetime. Multiply that times the value of max_frac_of_lifetime_per_step to get max_timestep.

set_max_dt_to_frac_lifetime = .false.
max_frac_of_lifetime_per_step = -1

astero_just_call_my_extras_check_model#

Communications flag for astero and star.

astero_just_call_my_extras_check_model = .false.

num_steps_for_garbage_collection#

If > 0 then every num_steps_for_garbage_collection steps we call the garbage collector This will try to free some memory from data structures that are no longer needed but have not been deallocated yet. There is no guarantee though that this will save memory and may slow your code down with additional deallocations/allocations.

For now this primarily targets the EOS data structures.

num_steps_for_garbage_collection = 0

report_garbage_collection#

Whether to print debug information about the garbage collector, output is printed both when mod(model_number,num_steps_for_garbage_collection)==0 and when mod(model_number-1,num_steps_for_garbage_collection)==0 (the next step) only runs if num_steps_for_garbage_collection > 0

report_garbage_collection = .false.

include other inlists#

You can split your star_job inlist into pieces using the following controls. BTW: it works recursively, so the extras can read extras too.

read_extra_star_job_inlist(1..5)#

extra_star_job_inlist_name(1..5)#

if read_extra_star_job_inlist(i) is true, then read &star_job from this namelist file

read_extra_star_job_inlist(:) = .false.
extra_star_job_inlist_name(:) = 'undefined'

save_star_job_namelist#

dumps all values for &star_job controls to file

save_star_job_namelist = .false.

star_job_namelist_name#

if empty, uses a default name

star_job_namelist_name = ''

private or experimental#

warn_run_star_extras#

Due to changing the run_star_extras functions to hooks, we break existing run_star_extras files. This flag sets a warning message and stops the MESA run until it is set to .false.. This way people will hopefully not be confused as to why their run_star_extras functions are not being called.

warn_run_star_extras = .true.

do_special_test#

do_special_test = .false.

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