controls

specifications for starting model

NOTE: if you are loading a saved model, then the following initial values are NOT USED to modify the model. in particular, you cannot use these to change Y or Z of an existing model. if you want to do that, see star_job.defaults controls such as change_Y. however, these are reported in output as the initial values for the star.

initial_mass

initial mass in Msun units. can be any value you’d like when you are creating a pre-main sequence model.

NOTE: this is not used when loading a saved model. however is reported in output as the initial mass of the star. don’t let that confuse you.

if you are loading a ZAMS model and the requested mass is in the range of prebuilt models, the code will interpolate in mass using the closest prebuilt models. if the requested mass is beyond the range of the prebuilt models, the code will load the closest one and then call “relax mass” to create a model to match the request. the prebuilt range is 0.08 Msun to 100 Msun, so the relax_mass method is only used for extreme cases. there are enough prebuilt models that the interpolation in mass seems to work fine for many applications.

initial_mass = 1

initial_z

initial metallicity for create pre-ms and create initial model initial_z can be any value from 0 to 0.04

not used when loading a saved model. however is reported in output as the initial Z of the star.

however, if you are loading a zams model, then initial_z must match one of the prebuilt values. look in the 'data/star_data/zams_models' directory to see what prebuilt zams Z’s are available. at time of writing, only 0.02 was included in the standard version of star.

initial_z = 0.02d0

initial_y

initial helium mass fraction for create pre-ms and create initial (< 0 means use default which is 0.24 + 2*initial_z)

not used when loading a saved model or a zams model. however is reported in output as the initial Y of the star.

NOTE: this is only used for create pre-main-sequence model and create initial model, and not when loading a zams model.

initial_y = -1

initial_he3

initial mass fraction of he3. Must be smaller than initial_y. (< 0 means use default which is taken as solar scaled such that he4/he3 has the same value as the Sun)

not used when loading a saved model or a zams model.

initial_he3 = -1

controls for output

terminal_interval

write info to terminal when mod(model_number, terminal_interval) = 0. note: this replaces the obsolete control terminal_cnt.

terminal_interval = 1

write_header_frequency

output the log header info to the terminal when mod(model_number, write_header_frequency*terminal_interval) = 0.

write_header_frequency = 10

extra_terminal_output_file

if not empty, output terminal info to this file in addition to terminal. this does not capture all of the terminal output – just the common items. it is intended for use in situations where you cannot directly see the terminal output such as when running on a cluster. if you want to be able to monitor the progress for such cases, you can set extra_terminal_output_file = 'log' and then do tail -f log to view the terminal output as it is recorded in the file.

extra_terminal_output_file = ''

terminal_show_age_units

terminal_show_timestep_units

terminal_show_log_dt

terminal_show_log_age

options are ‘years’, ‘yrs’, ‘days’, ‘secs’, or ‘seconds’ this replaces the old controls terminal_show_age_in_years & terminal_show_age_in_days

terminal_show_age_units = 'years'
terminal_show_timestep_units = 'years'
terminal_show_log_dt = .true.
terminal_show_log_age = .false.

num_trace_history_values

any valid name for a history data column, such as surf_v_rot for example if you have rapid rotation at the surface, you might want to try something like this:

num_trace_history_values = 7
trace_history_value_name(1) = 'surf_v_rot'
trace_history_value_name(2) = 'surf_omega_div_omega_crit'
trace_history_value_name(3) = 'log_rotational_mdot_boost'
trace_history_value_name(4) = 'log_total_angular_momentum'
trace_history_value_name(5) = 'center n14'
trace_history_value_name(6) = 'surface n14'
trace_history_value_name(7) = 'average n14'

value must be less than or equal to 10

num_trace_history_values = 0

trace_history_value_name(:)

write values to terminal

trace_history_value_name(:) = ''

photo_directory

directory for binary snapshots used in restarts

photo_directory = 'photos'

photo_interval

save a photo file for possible restarting when mod(model_number, photo_interval) = 0. note: this replaces the obsolete control photostep.

photo_interval = 50

photo_digits

use this many digits from the end of the model_number for the photo name

photo_digits = 3

log_directory

directory for data files about the run

log_directory = 'LOGS'

do_history_file

a history file is created if this is true

do_history_file = .true.

history_interval

append an entry to the history.data file when mod(model_number, history_interval) = 0.

history_interval = 5

star_history_name

name of history file

star_history_name = 'history.data'

star_history_header_name

If not empty, then put star history header info in star_history_name file. In this case the history file has only data, making it easier to use with some plotting packages.

star_history_header_name = ''

star_history_dbl_format

format for writing reals to star_history_name file

star_history_dbl_format = '(1pes40.16e3, 1x)'

star_history_int_format

format for writing integer to star_history_name file

star_history_int_format = '(i40, 1x)'

star_history_txt_format

format for writing characters to star_history_name file

star_history_txt_format = '(a40, 1x)'

write_profiles_flag

profiles are written only if this is true

write_profiles_flag = .true.

profile_interval

save a model profile info when mod(model_number, profile_interval) = 0.

profile_interval = 50

priority_profile_interval

give saved profile a higher priority for retention when mod(model_number, priority_profile_interval) = 0.

priority_profile_interval = 1000

profiles_index_name

name of the profile index file

profiles_index_name = 'profiles.index'

profiles_data_prefix

prefix of the profile data

profile_data_prefix = 'profile'

profiles_data_suffix

suffix of the profile data

profile_data_suffix = '.data'

profile_data_header_suffix

If not empty, then put profile data header info here. In this case the profile data file has only data, making it easier to use with some plotting packages.

profile_data_header_suffix = ''

profile_dbl_format

format for writing reals to profile file

profile_dbl_format = '(1pes40.16e3, 1x)'

profile_int_format

format for writing integers to profile file

profile_int_format = '(i40, 1x)'

profile_txt_format

format for writing characters to profile file

profile_txt_format = '(a40, 1x)'

max_num_profile_zones

if nz > this, then only write a subsample of the zones. only used if > 1

max_num_profile_zones = -1

max_num_profile_models

Maximum number of saved profiles. If there’s no limit on the number of profiles saved, you can fill up your disk – I’ve done it. So it’s a good idea to set this limit to a reasonable number such as 20 or 30. Once that many have been saved during a run, old ones will be discarded to make room for new ones. Profiles that were saved for key events are given priority and aren’t removed as long as there is a lower priority profile that can be discarded instead. Less than zero means no limit.

max_num_profile_models = 100

profile_model

save profile when model_number equals this

profile_model = -1

profile_header_include_sys_details

if this is true, profile header includes strings for compiler, build, etc.

profile_header_include_sys_details = .true.

write_model_with_profile

if this is true, models are written at same time as profiles

write_model_with_profile = .false.

model_data_prefix

prefix of the model data files

model_data_prefix = 'profile'

model_data_suffix

suffix of the model data files

model_data_suffix = '.mod'

write_controls_info_with_profile

if this is true, the values of the options in the controls inlist are written at same time as profiles

write_controls_info_with_profile = .false.

controls_data_prefix

prefix of the control data files

controls_data_prefix = 'controls'

controls_data_suffix

suffix of the control data files

controls_data_suffix = '.data'

mixing_D_limit_for_log

if max D_mix in mixing region is less than this, don’t include the region in the log doesn’t apply to thermohaline or semiconvective regions

mixing_D_limit_for_log = 1d4

write_pulse_data_with_profile

If .true., also save model data in a format compatible with pulsation codes.

write_pulse_data_with_profile = .false.

pulse_data_format

Format of pulsation data. Current options (case insensitive) are:

'CAFEIN'

Format defined for CAFein (Valsecchi et al. 2013).

'FGONG'

Format originally defined for the GONG solar model project. A definition was given in 2005 for the CoRoT/ESTA project and GONG itself. MESA’s implementation largely follows this subsequent 2015 definition.

'OSC'

Format similar to FGONG originally produced for models from CESAM. Also defined for the CoRoT/ESTA project.

'GYRE'

The plain-text format defined for GYRE, which GYRE itself refers to as 'MESA' format.

'GSM'

The HDF5-based format defined for GYRE.

'SAIO'

Format for Saio’s pulsation code.

'GR1D'

Format for GR1D, defined in Sec. 3 of the GR1D documentation.

pulse_data_format = 'FGONG'

add_atmosphere_to_pulse_data

if true, write atmosphere to pulse files. This is not valid when atm_option = 'table'

add_atmosphere_to_pulse_data = .false.

add_center_point_to_pulse_data

if true, add point for r=0 to pulse files

add_center_point_to_pulse_data = .true.

keep_surface_point_for_pulse_data

if true, add k=1 cell to pulse files

keep_surface_point_for_pulse_data = .false.

add_double_points_to_pulse_data

add double points at discontinuities

add_double_points_to_pulse_data = .false.

interpolate_rho_for_pulse_data

If true, then get rho_face by interpolating rho at cell center. If false, then calculate rho_face by dm/(4*pi*r^2*dr).

interpolate_rho_for_pulse_data = .true.

threshold_grad_mu_for_double_point

threshold in grad_mu = dln(mu)/dln(P) for a double point to be written

threshold_grad_mu_for_double_point = 10d0

max_number_of_double_points

maximum number of double points to be written (0 = no limit); when this limit is set, double points are chosen in order of decreasing \(|\nabla_\mu|\)

max_number_of_double_points = 0

fgong_header

These are the four lines of arbitrary text that appear at the beginning of an FGONG file to describe its contents.

fgong_header(1) = 'FGONG file'
fgong_header(2) = 'Created by MESAstar'
fgong_header(3) = ''
fgong_header(4) = ''

fgong_ivers

The version number for the FGONG file, which can only be 300 or 1300. 300 gives the old narrow format '(1P5E16.9,x)', which can produce numbers with no space separating them. 1300 gives the ‘wide’ FGONG format '(1P,5(X,E26.18E3))', as agreed on at the 5th Aarhus RGB workshop (University of Birmingham, UK, October 2015).

fgong_ivers = 1300 ! 300 or 1300 only

format_for_OSC_data

float format for 'OSC' data format

format_for_OSC_data = '(1P5E19.12,x)'

gyre_data_schema

data schema to use when passing model internally to GYRE, and/or writing files in GYRE/GSM format. For instance, to write v1.20 GYRE files use the value 120

gyre_data_schema = 101

max_num_gyre_points

limit gyre output files to at most this number of points only used when > 1

max_num_gyre_points = -1

fgong_zero_A_inside_r

when writing FGONG, if r < this and cell has mixing of some kind, force A = 0 Rsun units

fgong_zero_A_inside_r = 0d0

trace_mass_location

location for trace_mass_radius, trace_mass_logT, etc. (Msun units)

trace_mass_location = 0

min_tau_for_max_abs_v_location

controls choice of location in model for max_abs_v history info. can use this to exclude locations too close to surface. ignore if <= 0

min_tau_for_max_abs_v_location = 0

min_q_for_inner_mach1_location

controls choice of location in model for innermost mach 1 history info. can use this to exclude locations too close to center.

min_q_for_inner_mach1_location = 0

max_q_for_outer_mach1_location

controls choice of location in model for outermost mach 1 history info. can use this to exclude locations too close to surface.

max_q_for_outer_mach1_location = 1

burn_min1

used for reporting where burning zone occur, for example in the pgstar TRho profiles. see star/public/star_data.inc for details. must be < burn_min2. In ergs/g/sec.

burn_min1 = 50

burn_min2

used for reporting where burning zone occur, for example in the pgstar TRho profiles. see star/public/star_data.inc for details. In ergs/g/sec.

burn_min2 = 1000

width_for_limit_conv_vel

look this number of cells on either side of boundary to see if any boundary k in that range has s% csound(k) < s% v(k) <= s% csound(k-1) i.e. transition from subsonic to supersonic as go inward if find any such transition then don’t allow increase in convection velocity. this implies no change from radiative to convective. the purpose of this is to prevent convective energy transport from moving energy from behind a shock to in front of the shock.

width_for_limit_conv_vel = 3

max_q_for_limit_conv_vel

for q(k) <= this, don’t allow conv_vel to grow

max_q_for_limit_conv_vel = -1

max_r_in_cm_for_limit_conv_vel

for r(k) <= this, don’t allow conv_vel to grow

max_r_in_cm_for_limit_conv_vel = -1

max_mass_in_gm_for_limit_conv_vel

for m(k) <= this, don’t allow conv_vel to grow

max_mass_in_gm_for_limit_conv_vel = -1

center_avg_value_dq

reported center values are averages over this fraction of star mass

center_avg_value_dq = 1d-8

surface_avg_abundance_dq

reported surface abundances are averages over this fraction of star mass

surface_avg_abundance_dq = 1d-8

conv_core_gap_dq_limit

skip non-convective gaps of less than this limit when reporting convective core size

conv_core_gap_dq_limit = 0d0

definition of core boundaries

he_core_boundary_h1_fraction

If fraction >= 0, boundary is outermost location where h1 mass fraction is <= this value, and he4 mass fraction >= min_boundary_fraction (see below). If fraction < 0, boundary is outermost location where he4 is the most abundant species.

he_core_boundary_h1_fraction = 0.1d0

co_core_boundary_he4_fraction

If fraction >= 0, boundary is outermost location where he4 mass fraction is <= this value, and c12+o16 mass fraction >= min_boundary_fraction (see below). If fraction < 0, boundary is outermost location where c12+o16 is more abundant than any other species.

co_core_boundary_he4_fraction = 0.1d0

one_core_boundary_he4_c12_fraction

If fraction >= 0, boundary is outermost location where combine he4+c12 mass fraction is <= this value, and o16+ne20 mass fraction >= min_boundary_fraction (see below). If fraction < 0, boundary is outermost location where o16+ne20 is more abundant than any other species.

one_core_boundary_he4_c12_fraction = 0.1d0

fe_core_boundary_si28_fraction

For this case, “iron” includes any species with A > 46. If fraction >= 0, boundary is outermost location where si28 mass fraction is <= this value, and “iron” mass fraction >= min_boundary_fraction (see below). If fraction < 0, boundary is outermost location where “iron” is the most abundant species.

fe_core_boundary_si28_fraction = 0.1d0

neutron_rich_core_boundary_Ye_max

Boundary is outermost location where Ye is <= this value.

neutron_rich_core_boundary_Ye_max = 0.48d0

min_boundary_fraction

Value for deciding boundary regions.

min_boundary_fraction = 0.1d0

when to stop

max_model_number

The code will stop when it reaches this model number. Negative means no maximum.

max_model_number = -1

when_to_stop_rtol

when_to_stop_atol

Relative (rtol) and absolute (atol) error criteria for target stopping values. To compare how accurately the last step satisfied a stopping condition, MESA evaluates

error = abs(value - target_value)/ &
        (when_to_stop_atol + when_to_stop_rtol*max(abs(value), abs(target_value)))

and will redo with a smaller timestep if error is greater than 1. The default values 1d99 for both guarantee that error is tiny, so the run terminates as soon as a stopping condition is reached.

If you wish to use either rtol or atol, you should change the other to 0 (or your desired value). To see why, suppose we only set when_to_stop_rtol = 1d-3. Because when_to_stop_atol is still 1d99, error will still be very small and MESA won’t redo the last step.

when_to_stop_rtol = 1d99
when_to_stop_atol = 1d99

max_age

max_age_in_days

max_age_in_seconds

Stop when the age of the star exceeds this value in years, days, or seconds. Only applies when > 0.

max_age = 1d36
max_age_in_days = -1
max_age_in_seconds = -1

num_adjusted_dt_steps_before_max_age

This adjusts max_years_for_timestep so that hit max_age exactly, without needing possibly large change in timestep at end of run. only used if > 0

number of time steps to adjust to prior to hitting max age only used if > 0

num_adjusted_dt_steps_before_max_age = 0

dt_years_for_steps_before_max_age

timestep in years

dt_years_for_steps_before_max_age = 1d6

reduction_factor_for_max_timestep

per time step reduction limited to this

reduction_factor_for_max_timestep = 0.98d0

gamma_center_limit

gamma is the plasma interaction parameter. Stop when the center value of gamma exceeds this limit.

gamma_center_limit = 1d99

eta_center_limit

eta is the electron chemical potential in units of k*T. Stop when the center value of eta exceeds this limit.

eta_center_limit = 1d99

log_center_density_upper_limit

log_center_density_lower_limit

Stop when log10 of the center density is above/below the upper/lower limit.

log_center_density_upper_limit = 12d0
log_center_density_lower_limit = -1d99

log_center_temp_upper_limit

log_center_temp_lower_limit

Stop when log10 of the center temperature is above/below the upper/lower limit.

log_center_temp_upper_limit = 11d0
log_center_temp_lower_limit = -1d99

surface_accel_div_grav_limit = -1

This is used when do not have a velocity variable. The acceleration ratio is abs(accel)/grav at surface, where accel is (rdot-rdot_old)/dt and grav is G*m/r^2. Stop if the ratio becomes larger than this limit. Ignored if <= 0.

surface_accel_div_grav_limit = -1

log_max_temp_upper_limit

log_max_temp_lower_limit

stop when log10 of the maximum temperature is above/below the upper/lower limit.

log_max_temp_upper_limit = 99
log_max_temp_lower_limit = -99

center_entropy_upper_limit

center_entropy_lower_limit

stop when the center entropy is above/below the upper/lower limit. in kerg per baryon, where kerg = (erg K^-1)

center_entropy_upper_limit = 1d99
center_entropy_lower_limit = -1d99

max_entropy_upper_limit

max_entropy_lower_limit

stop when the max entropy is above/below the upper/lower limit. in kerg per baryon, where kerg = (erg K^-1)

max_entropy_upper_limit = 1d99
max_entropy_lower_limit = -1d99

xa_central_lower_limit_species

xa_central_lower_limit

Lower limits on central mass fractions. Stop when central abundance drops below this limit. Can have up to num_xa_central_limits of these (see star_def.inc for value). xa_central_lower_limit_species contains an isotope name as defined in chem_def.f90. xa_central_lower_limit contains the lower limit value.

xa_central_lower_limit_species(1) = ''
xa_central_lower_limit(1) = 0

xa_central_upper_limit_species

xa_central_upper_limit

Upper limits on central mass fractions. Stop when central abundance rises above this limit. Can have up to num_xa_central_limits of these (see star_def.inc for value). E.g., to stop when center c12 abundance reaches 0.5, set

xa_central_upper_limit_species(1) = 'c12'
xa_central_upper_limit(1) = 0.5

xa_central_upper_limit_species(1) = ''
xa_central_upper_limit(1) = 0

xa_surface_lower_limit_species

xa_surface_lower_limit

Lower limits on surface mass fractions. Stop when surface abundance drops below this limit. Can have up to num_xa_surface_limits of these (see star_def for value) xa_surface_lower_limit_species contains an isotope name as defined in chem_def.f90 xa_surface_lower_limit contains the lower limit value

xa_surface_lower_limit_species(1) = ''
xa_surface_lower_limit(1) = 0

xa_surface_upper_limit_species

xa_surface_upper_limit

upper limits on surface mass fractions stop when surface abundance rises above this limit can have up to num_xa_surface_limits of these (see star_def for value) e.g., to stop when surface c12 abundance reaches 0.5, set

xa_surface_upper_limit_species(1) = 'c12'
xa_surface_upper_limit(1) = 0.5

xa_surface_upper_limit_species(1) = ''
xa_surface_upper_limit(1) = 0

xa_average_lower_limit_species

xa_average_lower_limit

lower limits on average mass fractions stop when average abundance drops below this limit can have up to num_xa_average_limits of these (see star_def for value)

xa_average_lower_limit_species(1) = ''
xa_average_lower_limit(1) = 0

xa_average_upper_limit_species

xa_average_upper_limit

upper limits on average mass fractions stop when average abundance rises above this limit can have up to num_xa_average_limits of these (see star_def for value)

xa_average_upper_limit_species(1) = ''
xa_average_upper_limit(1) = 0

HB_limit

For detecting when the model has completed the horizontal branch. Only applies when center abundance by mass of h1 is < 1d-4. Stop when the center abundance by mass of he4 drops below this limit.

HB_limit = 0

star_mass_min_limit

Stop when star mass in Msun units is < this. <= 0 means no limit.

star_mass_min_limit = 0

star_mass_max_limit

Stop when star mass in Msun units is > this. <= 0 means no limit.

star_mass_max_limit = 0

remnant_mass_min_limit

ejecta_mass_max_limit

Stop when remnant mass in Msun units is < this. <= 0 means no limit. remnant_mass = star_mass - ejecta_mass ejecta_mass is outermost mass that all has v(k) >= v_escape(k)

remnant_mass_min_limit = 0
ejecta_mass_max_limit = 1d99

star_species_mass_min_limit

star_species_mass_min_limit_iso

star_species_mass_max_limit

star_species_mass_max_limit_iso

Stop when a particular species mass in units of Msun exceeds these limits.

star_species_mass_min_limit = 0
star_species_mass_min_limit_iso = ''

star_species_mass_max_limit = 0
star_species_mass_max_limit_iso = ''

star_H_mass_max_limit

Stop when star hydrogen mass in Msun units is > this. <= 0 means no limit.

star_H_mass_min_limit replaced by star_species_mass_min_limit star_He_mass_min_limit replaced by star_species_mass_min_limit star_C_mass_min_limit replaced by star_species_mass_min_limit star_H_mass_max_limit replaced by star_species_mass_max_limit star_He_mass_max_limit replaced by star_species_mass_max_limit star_C_mass_max_limit replaced by star_species_mass_max_limit

envelope_mass_limit

envelope_mass = star_mass - he_core_mass

Stop when envelope_mass drops below this limit, in Msun units.

envelope_mass_limit = 0

envelope_fraction_left_limit

envelope_fraction_left = (star_mass - he_core_mass)/(initial_mass - he_core_mass)

Stop when envelope_fraction_left < this limit.

envelope_fraction_left_limit = 0

xmstar_min_limit

xmstar = mstar - M_center

stop when xmstar in grams is < this. <= 0 means no limit.

xmstar_min_limit = 0

xmstar_max_limit

xmstar = mstar - M_center

stop when xmstar in grams is > this. <= 0 means no limit.

xmstar_max_limit = 0

he_core_mass_limit

stop when helium core reaches this mass, in Msun units

he_core_mass_limit = 1d99

co_core_mass_limit

stop when CO core reaches this mass, in Msun units

co_core_mass_limit = 1d99

one_core_mass_limit

stop when ONe core reaches this mass, in Msun units

one_core_mass_limit = 1d99

fe_core_mass_limit

stop when iron core reaches this mass, in Msun units

fe_core_mass_limit = 1d99

neutron_rich_core_mass_limit

stop when neutron rich core reaches this mass, in Msun units

neutron_rich_core_mass_limit = 1d99

he_layer_mass_lower_limit

he layer mass is defined as he_core_mass - c_core_mass stop when c_core_mass > 0 and he layer mass < this limit (Msun units).

he_layer_mass_lower_limit = 0

abs_diff_lg_LH_lg_Ls_limit

stop when abs(lg_LH - lg_Ls) <= abs_diff_LH_Lsurf_limit can be useful for deciding when pre-main sequence star has reached ZAMS set to negative value to disable

abs_diff_lg_LH_lg_Ls_limit = -1

Teff_upper_limit

stop when Teff is greater than this limit.

Teff_upper_limit = 1d99

Teff_lower_limit

stop when Teff is less than this limit.

Teff_lower_limit = -1d99

photosphere_r_upper_limit

stop when photosphere_r is greater than this limit, in Rsun units

photosphere_r_upper_limit = 1d99

photosphere_r_lower_limit

stop when photosphere_r is less than this limit, in Rsun units

photosphere_r_lower_limit = -1d99

photosphere_m_upper_limit

stop when photosphere_m is greater than this limit, in Msun units

photosphere_m_upper_limit = 1d99

photosphere_m_lower_limit

stop when photosphere_m is less than this limit, in Msun units

photosphere_m_lower_limit = -1d99

photosphere_m_sub_M_center_limit

stop when photosphere_m is less than this limit above M_center, in Msun units

photosphere_m_sub_M_center_limit = -1d99

log_Teff_upper_limit

stop when log10 of Teff is greater than this limit.

log_Teff_upper_limit = 1d99

log_Teff_lower_limit

stop when log10 of Teff is less than this limit.

log_Teff_lower_limit = -1d99

log_Tsurf_upper_limit

stop when log10 of T in outermost cell is greater than this limit.

log_Tsurf_upper_limit = 1d99

log_Tsurf_lower_limit

stop when log10 of T in outermost cell is less than this limit.

log_Tsurf_lower_limit = -1d99

log_Rsurf_upper_limit

stop when log10 of R/Rsun in outermost cell is greater than this limit.

log_Rsurf_upper_limit = 1d99

log_Rsurf_lower_limit

stop when log10 of R/Rsun in outermost cell is less than this limit.

log_Rsurf_lower_limit = -1d99

log_L_upper_limit

stop when log10(total luminosity in Lsun units) is greater than this limit. in order to skip pre-ms, this limit only applies when L_nuc > 0.01*L

log_L_upper_limit = 1d99

log_L_lower_limit

stop when log10(total luminosity in Lsun units) is less than this limit.

log_L_lower_limit = -1d99

log_g_upper_limit

stop when log10(gravity at surface) is greater than this limit.

log_g_upper_limit = 1d99

log_g_lower_limit

stop when log10(gravity at surface) is less than this limit.

log_g_lower_limit = -1d99

log_Psurf_upper_limit

stop when log10 of surface pressure is greater than this limit.

log_Psurf_upper_limit = 1d99

log_Psurf_lower_limit

stop when log10 of surface pressure is less than this limit.

log_Psurf_lower_limit = -1d99

log_Dsurf_upper_limit

stop when log10 of surface density is greater than this limit.

log_Dsurf_upper_limit = 1d99

log_Dsurf_lower_limit

stop when log10 of surface density is less than this limit.

log_Dsurf_lower_limit = -1d99

power_nuc_burn_upper_limit

stop when total power from all nuclear reactions (in Lsun units) is > this.

power_nuc_burn_upper_limit = 1d99

power_h_burn_upper_limit

stop when total power from hydrogen-consuming reactions (in Lsun units) is > this.

power_h_burn_upper_limit = 1d99

power_he_burn_upper_limit

stop when total power from reactions burning helium (in Lsun units) is > this.

power_he_burn_upper_limit = 1d99

power_z_burn_upper_limit

stop when total power from reactions burning metals (in Lsun units) is > this

power_z_burn_upper_limit = 1d99

power_nuc_burn_lower_limit

stop when total power from all nuclear reactions (in Lsun units) is < this.

power_nuc_burn_lower_limit = -1d99

power_h_burn_lower_limit

stop when total power from hydrogen consuming reactions (in Lsun units) is < this.

power_h_burn_lower_limit = -1d99

power_he_burn_lower_limit

stop when total power from reactions burning helium (in Lsun units) is < this.

power_he_burn_lower_limit = -1d99

power_z_burn_lower_limit

stop when total power from reactions burning metals (in Lsun units) is < this.

power_z_burn_lower_limit = -1d99

max_abs_rel_run_E_err

Stop if the abs value of cumulative_energy_error/total_energy exceeds this value. Ignore if < 0. Also ignore during relax operations.

max_abs_rel_run_E_err = -1

max_number_retries

Stop if the number of retries exceeds this value. Ignore if < 0.

max_number_retries = -1

relax_max_number_retries = 300

min_timestep_limit

stop if need timestep smaller than this limit, in seconds

min_timestep_limit = 1d-6

center_Ye_lower_limit

stop if center_ye drops below this limit

center_Ye_lower_limit = -1

center_R_lower_limit

stop if R_center drops below this limit (in cm)

center_R_lower_limit = -1

fe_core_infall_limit

stop if at least fe_core_infall_mass of material has speed greater than this, at a location interior to fe_core_mass, in cm/s

fe_core_infall_limit = 3d7

fe_core_infall_mass

Amount of mass to check if collapsing, the smaller this is the closer the velocity minima will be to fe_core_infall but there will be a greater chance of a transistent velocity spike causing the model to prematurely exit. In solar masses

fe_core_infall_mass = 0.1d0

non_fe_core_infall_limit

stop if at least non_fe_core_infall_mass of material has speed greater than this, at a location interior to he_core_mass and exterior to fe_core_mass. in cm/s

non_fe_core_infall_limit = 1d99

non_fe_core_infall_mass

Amount of mass to check if collapsing, the smaller this is the closer the velocity minima will be to non_fe_core_infall but there will be a greater chance of a transistent velocity spike causing the model to prematurely exit. In solar masses

non_fe_core_infall_mass = 0.1d0

non_fe_core_rebound_limit

stop if max rebound speed (outward) at any location interior to he_core_mass. in cm/s

non_fe_core_rebound_limit = 1d99

v_div_csound_max_limit

stop if any v/csound > this limit

v_div_csound_max_limit = 1d99

v_div_csound_surf_limit

stop if v_surf/csound_surf > this limit

v_div_csound_surf_limit = 1d99

v_surf_div_v_kh_upper_limit

stop if abs(v_surf/v_kh) > this limit, where v_kh = photosphere_r/kh_timescale

v_surf_div_v_kh_upper_limit = 1d99

v_surf_div_v_kh_lower_limit

stop if abs(v_surf/v_kh) < this limit, where v_kh = photosphere_r/kh_timescale

v_surf_div_v_kh_lower_limit = -1d99

v_surf_div_v_esc_limit

stop if v_surf/v_esc > this limit

v_surf_div_v_esc_limit = 1d99

v_surf_kms_limit

stop if v_surf in km/s > this limit

v_surf_kms_limit = 1d99

Lnuc_div_L_zams_limit

defines “near zams” – note: must also set stop_near_zams

Lnuc_div_L_zams_limit = 0.9d0

stop_near_zams

if true, stop if Lnuc/L > Lnuc_div_L_zams_limit

stop_near_zams = .false.

stop_at_phase_PreMS

stop_at_phase_ZAMS

stop_at_phase_IAMS

stop_at_phase_TAMS

stop_at_phase_He_Burn

stop_at_phase_ZACHeB

stop_at_phase_TACHeB

stop_at_phase_TP_AGB

stop_at_phase_C_Burn

stop_at_phase_Ne_Burn

stop_at_phase_O_Burn

stop_at_phase_Si_Burn

stop_at_phase_WDCS

if true, terminate model when phase of evolution reaches this point. Definitions for stop_at_phase_* can be found in $MESA_DIR/star/private/star_utils.f90 inside the subroutine set_phase_of_evolution

::

stop_at_phase_PreMS = .false. stop_at_phase_ZAMS = .false. stop_at_phase_IAMS = .false. stop_at_phase_TAMS = .false. stop_at_phase_He_Burn = .false. stop_at_phase_ZACHeB = .false. stop_at_phase_TACHeB = .false. stop_at_phase_TP_AGB = .false. stop_at_phase_C_Burn = .false. stop_at_phase_Ne_Burn = .false. stop_at_phase_O_Burn = .false. stop_at_phase_Si_Burn = .false. stop_at_phase_WDCS = .false.

Lnuc_div_L_upper_limit

stop when Lnuc/L is greater than this limit. Here, Lnuc refers to the total thermal power from all burning, including photodisintegrations, power_nuc_burn in the history_columns.list file. L is the luminosity at the photosphere.

Lnuc_div_L_upper_limit = 1d99

Lnuc_div_L_lower_limit

stop when Lnuc/L is less than this limit. Here, Lnuc refers to the total thermal power from all burning, including photodisintegrations, power_nuc_burn in the history_columns.list file. L is the luminosity at the photosphere.

Lnuc_div_L_lower_limit = -1d99

gamma1_limit

stop if min gamma1 < this limit in a cell with q <= gamma1_limit_max_q

gamma1_limit = -1

gamma1_limit_max_q

stop if gamma1 < this limit at any location with q <= gamma1_limit_max_q values near unity skip the outer envelope

gamma1_limit_max_q = 0.95d0

gamma1_limit_max_v_div_vesc

stop if gamma1 < this limit at any location with v_div_vesc <= gamma1_limit_max_v_div_vesc

gamma1_limit_max_v_div_vesc = 0.95d0

Pgas_div_P_limit

stop when Pgas/P <= Pgas_div_P_limit

Pgas_div_P_limit = 0

Pgas_div_P_limit_max_q

stop if Pgas/P < Pgas_div_P_limit at any location with q <= Pgas_div_P_limit_max_q values near unity skip the outer envelope

Pgas_div_P_limit_max_q = 0.95d0

peak_burn_vconv_div_cs_limit

limits ratio of convection velocity to sound speed at location of peak eps_nuc

peak_burn_vconv_div_cs_limit = 1d99

omega_div_omega_crit_limit

stop if omega/omega_crit is > this anywhere in star ignore if < 0

omega_div_omega_crit_limit = -1

delta_nu_lower_limit

stop when asteroseismology delta_nu in micro Hz is < this. <= 0 means no limit.

delta_nu_lower_limit = 0

delta_nu_upper_limit

stop when asteroseismology delta_nu in micro Hz is > this. <= 0 means no limit.

delta_nu_upper_limit = 0

shock_mass_upper_limit

stop when shock_mass is > this. <= 0 means no limit.

shock_mass_upper_limit = -1

mach1_mass_upper_limit

stop when outer location of mach 1 is > this. <= 0 means no limit.

mach1_mass_upper_limit = -1

delta_Pg_lower_limit

stop when delta_Pg in micro Hz is < this. <= 0 means no limit.

delta_Pg_lower_limit = 0

delta_Pg_upper_limit

stop when delta_Pg in micro Hz is > this. <= 0 means no limit.

delta_Pg_upper_limit = 0

stop_when_reach_this_cumulative_extra_heating

(ignore if <= 0)

stop_when_reach_this_cumulative_extra_heating = 0d0

mixing parameters

mixing_length_alpha

The mixing length is this parameter times a local pressure scale height. To increase R vs. L, decrease mixing_length_alpha.

mixing_length_alpha = 2

remove_small_D_limit

If MLT diffusion coeff D (cm^2/sec) is less than this limit, then set D to zero and change the point to mixing_type == no_mixing.

remove_small_D_limit = 1d-6

use_Ledoux_criterion

a location in the model is Schwarzschild stable when gradr < grada it is Ledoux stable when gradr < gradL, where gradL = grada + composition_gradient note that these are the same when composition_gradient = 0 so you can force the use of the Schwarzschild criterion by passing 0 for the composition_gradient argument to the mlt routine. that’s what happens if you set the control “use_Ledoux_criterion” to false.

overshooting and rotational mixing are dealt with separately

and are added after the MLT classifications are made.

use_Ledoux_criterion = .false.

num_cells_for_smooth_gradL_composition_term

Number of cells on either side to use in weighted smoothing of gradL_composition_term. gradL_composition_term is set to the “raw” unsmoothed brunt_B and then optionally smoothed according num_cells_for_smooth_gradL_composition_term. In cases where the Ledoux criterion is used to evaluate the boundary for burning convective cores, you may need to set num_cells_for_smooth_gradL_composition_term = 0 to avoid smoothing the stabilizing composition jump into the convection zone and unphysically causing it to shrink. See section 3.2 in Moore, K., & Garaud, P. 2016, APJ, 817, 54

num_cells_for_smooth_gradL_composition_term = 3

threshold_for_smooth_gradL_composition_term

Threshold for weighted smoothing of gradL_composition_term. Only apply smoothing (controlled by num_cells_for_smooth_gradL_composition_term) for contiguous regions where \(|\nabla_L|\) exceeds this threshold. Might be useful for preventing narrow composition jumps from being excessively broadened by smoothing

threshold_for_smooth_gradL_composition_term = 0

alpha_semiconvection

Determines efficiency of semiconvective mixing. Semiconvection only applies if use_Ledoux_criterion is true.

alpha_semiconvection = 0

semiconvection_option

• 'Langer_85 mixing; gradT = gradr' : uses Langer scheme for mixing but sets gradT = gradr

• 'Langer_85' : this calculates special gradT as well as doing mixing.

semiconvection_option = 'Langer_85 mixing; gradT = gradr'

thermohaline_coeff

Determines efficiency of thermohaline mixing. was previously named thermo_haline_coeff. thermohaline mixing only applies if use_Ledoux_criterion is true.

thermohaline_coeff = 0

thermohaline_option

determines which method to use for calculating thermohaline diffusion coef:

• 'Kippenhahn' : use method of Kippenhahn, R., Ruschenplatt, G., & Thomas, H.-C. 1980, A&A, 91, 175.

• 'Traxler_Garaud_Stellmach_11' : use method of Traxler, Garaud, & Stellmach, ApJ Letters, 728:L29 (2011).

• 'Brown_Garaud_Stellmach_13' : use method of Brown, Garaud, & Stellmach, ApJ 768:34 (2013) Recommends thermohaline_coeff = 1, but it can nevertheless be changed.

thermohaline_option = 'Kippenhahn'

alt_scale_height_flag

If false, then stick to the usual definition – P/(g*rho). If true, use min of the usual and sound speed * hydro time scale, sqrt(P/G)/rho. Note that the ‘TDC’ MLT_option does not respect the alt_scale_height option, and continues to use h = P / rho g even if that flag is set.

alt_scale_height_flag = .true.

mlt_use_rotation_correction

When doing rotation, multiply grad_rad by ft_rot/ft_rot if this flag is true.

mlt_use_rotation_correction = .true.

mlt_Pturb_factor

include MLT turbulent pressure at face k = mlt_Pturb_factor*0.5*(rho(k) + rho(k-1))*mlt_vc(k)**2/3 MLT turbulent pressure for cell k = avg of values at faces.

this replaces conv_dP_term_factor. also see extra_pressure vector and other_pressure routine

mlt_Pturb_factor = 0d0

MLT_option

Options are:

• ‘none’ : just give radiative values with no mixing.

• ‘TDC’ : Time-dependent convection based on the Khufuss 1986 model. Reduces to Cox at long times.

• ‘Cox’ : MLT as developed in Cox & Giuli 1968, Chapter 14.

• ‘ML1’ : Bohm-Vitense 1958

• ‘ML2’ : Bohm and Cassinelli 1971

• ‘Mihalas’ : Mihalas 1978, Kurucz 1979

• ‘Henyey’ : Henyey, Vardya, and Bodenheimer 1965

The ‘Cox’ and ‘TDC’ options assumes optically thick material. The other options are various ways of extending to include optically thin material. Note that TDC does not respect the alt_scale_height option, and continues to use h = P / rho g even if that flag is set.

We caution that combining different mixing models in a stellar evolution calculation might lead to physically inconsistent solutions, because the different models have been developed separately, and their underlying assumptions might not be compatible with each other. Examples include combining the newly implemented time-dependent local limit convection model TDC with an overshooting model, or combining TDC with other models for chemical composition gradients (predictive mixing or convective premixing), rotation, etc. (MESA VI)

MLT_option = 'TDC'

TDC options

• alpha_TDC_DAMP : The turbulent viscous damping parameter which determines the saturation of TDC. Increasing this decreases convection speeds.

• alpha_TDC_DAMPR : The radiative damping parameter which determines the saturation of TDC. Increasing this decreases convection speeds.

• alpha_TDC_PtdVdt : The prefactor on the term accounting for work done against turbulent pressure (P_turb * dV/dt). Physically this should be unity.

• steps_before_use_TDC : TDC often struggles with models on the pre-main-sequence. Set this option to pick MLT_option=’Cox’ for the first several steps to get past the pre-MS. Note that if this option is positive then only either TDC or Cox will be used (depending on model number). THIS OVERRIDES MLT_option!

alpha_TDC_DAMP = 1d0
alpha_TDC_DAMPR = 0d0
alpha_TDC_PtdVdt = 0d0
steps_before_use_TDC = 0

Henyey_MLT_y_param

Henyey_MLT_nu_param

Values of the f1..f4 coefficients are taken from Table 1 of Ludwig et al. 1999, A&A, 346, 111 with the following exception: their value of f3 for Henyey convection is f4/8 when it should be 8*f4, i.e., f3=32*pi**2/3 and f4=4*pi**2/3. f3 and f4 are related to the henyey y parameter, so for the ‘Henyey’ case they are set based on the value of Henyey_y_param.

Henyey_MLT_y_param = 0.33333333d0
Henyey_MLT_nu_param = 8

make_gradr_sticky_in_solver_iters

min_logT_for_make_gradr_sticky_in_solver_iters

if true, then location that becomes radiative during solver iterations, stays radiative for rest of the solver iterations. to avoid flip-flopping between radiative and convective. also do this if max logT >= min_logT_for_make_gradr_sticky_in_solver_iters

make_gradr_sticky_in_solver_iters = .false.
min_logT_for_make_gradr_sticky_in_solver_iters = 1d99

no_MLT_below_shock

if true, then no MLT below an outward going shock (just radiative).

no_MLT_below_shock = .false.

mlt_make_surface_no_mixing

mlt_make_surface_no_mixing = .false.

T_mix_limit

If there is any convection in surface zones with T < T_mix_limit, then extend the innermost such convective region outward all the way to the surface. For example,

• T_mix_limit <= 0 means omit this operation.

• T_mix_limit = 1d5 will effectively make the star convective down to the He++ region.

units in Kelvin

T_mix_limit = 0

mlt_gradT_fraction

let f := mlt_gradT_fraction if f is >= 0 and <= 1, then gradT from mlt is replaced by f*grada_at_face(k) + (1-f)*gradr(k) see also the vector control adjust_mlt_gradT_fraction for fine grain control

mlt_gradT_fraction = -1

okay_to_reduce_gradT_excess

gradT_excess = gradT_sub_grada = superadiabaticity.

Inefficient convection => large gradT excess and steep T gradient to enhance radiative transport. Reduce gradT excess by making gradT closer to adiabatic gradient. If true, code is allowed to adjust gradT to boost efficiency of energy transport See gradT_excess_f1, gradT_excess_f2, and gradT_excess_age_fraction below.

This is the treatment of convection, referred to as MLT++ in Section 7.2 of Paxton et al. (2013), that reduces the superadiabaticity in some radiation-dominated convective regions.

okay_to_reduce_gradT_excess = .false.

gradT_excess_f1

gradT_excess_f2

These are for calculation of efficiency boosted gradT.

gradT_excess_f1 = 1d-4
gradT_excess_f2 = 1d-3

gradT_excess_age_fraction

These are for calculation of efficiency boosted gradT. Fraction of old to mix with new to get next.

gradT_excess_age_fraction = 0.9d0

gradT_excess_max_change

These are for calculation of efficiency boosted gradT. Maximum change allowed in one timestep for gradT_excess_alpha. Ignored if negative.

gradT_excess_max_change = -1d0

gradT_excess_lambda1

gradT_excess_beta1

In some situations you might want to force alfa = 1. You can do that by setting gradT_excess_lambda1 < 0. The following are for the normal calculation of gradT_excess_alfa

gradT_excess_lambda1 = 1.0d0
gradT_excess_beta1 = 0.35d0

gradT_excess_lambda2

gradT_excess_beta2

The following are for the normal calculation of gradT_excess_alfa.

gradT_excess_lambda2 = 0.5d0
gradT_excess_beta2 = 0.25d0

gradT_excess_dlambda

gradT_excess_dbeta

The following are for the normal calculation of gradT_excess_alfa.

gradT_excess_dlambda = 0.1d0
gradT_excess_dbeta = 0.1d0

gradT_excess_max_center_h1

No boost if center H1 > this limit.

gradT_excess_max_center_h1 = 1d0

gradT_excess_min_center_he4

No boost if center He4 < this limit.

gradT_excess_min_center_he4 = 0d0

gradT_excess_max_logT

No local boost if local logT > this limit.

gradT_excess_max_logT = 8

gradT_excess_min_log_tau_full_on

gradT_excess_max_log_tau_full_off

No local boost if local log_tau < gradT_excess_max_log_tau_full_off. Reduced local boost if local log_tau < gradT_excess_min_log_tau_full_on.

gradT_excess_min_log_tau_full_on = -99
gradT_excess_max_log_tau_full_off = -99

### max_logT_for_mlt

No mlt at cell if local logT > this limit.

max_logT_for_mlt = 99

use_superad_reduction

superad_reduction_Gamma_limit

superad_reduction_Gamma_limit_scale

superad_reduction_Gamma_inv_scale

superad_reduction_diff_grads_limit

superad_reduction_limit

Implicit alternative to okay_to_reduce_gradT_excess

use_superad_reduction = .false.
superad_reduction_Gamma_limit = 0.5d0
superad_reduction_Gamma_limit_scale = 5d0
superad_reduction_Gamma_inv_scale = 5d0
superad_reduction_diff_grads_limit = 1d-3
superad_reduction_limit = -1d0

overshooting

There are two schemes implemented in MESA to treat overshooting: a step overshoot scheme and an exponential scheme.

Parameters for exponential diffusive overshoot are described in the paper by Falk Herwig, “The evolution of AGB stars with convective overshoot”, A&A, 360, 952-968 (2000).

Overshooting depends on the classification of the convective zone and can be different at the top and the bottom of the zone.

The overshooting controls are based on convection-zone and convection-boundary matching criteria. These criteria are overshoot_zone_type, overshoot_zone_loc and overshoot_bdy_loc. The overshooting parameter values corresponding to the first set of matching criteria will be used. Therefore, narrower criteria should precede more general ones (i.e have lower array indices).

These are arrays of size NUM_OVERSHOOT_PARAM_SETS which is defined in star_data/public/star_data_def.inc (currently 16)

overshoot_scheme(:) = '' ! ``exponential``, ``step``, ``other``
overshoot_zone_type(:) = '' !  ``burn_H``, ``burn_He``, ``burn_Z``, ``nonburn``, ``any``
overshoot_zone_loc(:) = '' ! ``core``, ``shell``, ``any``
overshoot_bdy_loc(:) = '' ! ``bottom``, ``top``, ``any``

Amount of overshooting from edge of convective zone These are arrays of size NUM_OVERSHOOT_PARAM_SETS which is defined in star_data/public/star_data_def.inc (currently 16)

overshoot_f(:) = 0d0
overshoot_f0(:) = 0d0

The switch from convective mixing to overshooting happens at a distance f0*Hp into the convection zone from the estimated location where grad_ad = grad_rad, where Hp is the pressure scale height at that location. A value <= 0 for f0 is a mistake – you are required to set f0 as well as f. take a look at the following from an email concerning this: Overshooting works by taking the diffusion mixing coefficient at the edge of the convection zone and extending it beyond the zone. But – and here’s the issue – at the exact edge of the zone the mixing coefficient goes to 0. So we don’t want that. Instead we want the value of the mixing coeff NEAR the edge, but not AT the edge. The “f0” parameter determines the exact meaning of “near” for this. It tells the code how far back into the zone to go in terms of scale height. The overshooting actually begins at the location determined by f0 back into the convection zone rather than at the edge where the diffusion coeff is ill-defined. So, for example, if you want overshooting of 0.2 scale heights beyond the normal edge, you might want to back up 0.05 scale heights to get the diffusion coeff from near the edge and then go out by 0.25 scale heights from there to reach 0.2 Hp beyond the old boundary. In the inlist this would mean setting the “f0” to 0.05 and the “f” to 0.25.

For step overshoot: overshooting extends a distance overshoot_f*Hp0 from r0 with constant diffusion coefficient D = overshoot_D0 + overshoot_Delta0*D_ob where D_ob is the convective diffusivity at the bottom (top) of the step overshoot region for outward (inward) overshooting. These are arrays of size NUM_OVERSHOOT_PARAM_SETS which is defined in star_data/public/star_data_def.inc (currently 16)

overshoot_D0(:) = 0d0
overshoot_Delta0(:) = 1d0

You can specify a range of star masses over which overshooting above H burning zones is gradually enabled. Do specified overshooting above H burning zone if star_mass >= this (Msun). These are arrays of size NUM_OVERSHOOT_PARAM_SETS which is defined in star_data/public/star_data_def.inc (currently 16)

overshoot_mass_full_on(:) = 0d0

You can specify a range of star masses over which overshooting above H burning zones is gradually enabled. No overshooting above H burning zone if star_mass <= this (Msun). These are arrays of size NUM_OVERSHOOT_PARAM_SETS which is defined in star_data/public/star_data_def.inc (currently 16)

overshoot_mass_full_off(:) = 0d0

overshoot_D_min

Overshooting shuts off when the exponential decay has dropped the diffusion coefficient to this level.

overshoot_D_min = 1d2

overshoot_brunt_B_max

Terminate overshoot region when encounter stabilizing composition gradient where (unsmoothed) brunt_B is greater than this limit. (<= 0 means ignore this limit) note: both brunt_B and gradL_composition_term come from unsmoothed_brunt_B and differ only in optional smoothing. (see num_cells_for_smooth_brunt_B and num_cells_for_smooth_gradL_composition_term).

overshoot_brunt_B_max = 0d0

min_overshoot_q

Overshooting is only allowed at locations with mass m >= min_overshoot_q * mstar. E.g., if min_overshoot_q = 0.1, then only the outer 90% by mass can have overshooting. This provides a simple way of suppressing bogus center overshooting in which a small convective region at the core can produce excessively large overshooting because of a large pressure scale height at the center.

min_overshoot_q = 0d0

NOTE: In addition to giving these ‘f’ parameters non-zero values, you should also check the settings for mass_for_overshoot_full_on and mass_for_overshoot_full_off.

overshoot_alpha

The value of Hp for overshooting is limited to the radial thickness of the convection zone divided by overshoot_alpha. only used when > 0. if <= 0, then use mixing_length_alpha instead.

overshoot_alpha = -1

limit_overshoot_Hp_using_size_of_convection_zone

if false, allow large distance of overshoot for small convective zones.

limit_overshoot_Hp_using_size_of_convection_zone = .true.

burn_z_mix_region_logT

burn_he_mix_region_logT

burn_h_mix_region_logT

max logT in convective region determines burn type for overshooting

burn_z_mix_region_logT = 8.7d0
burn_he_mix_region_logT = 7.7d0
burn_h_mix_region_logT = 6.7d0

max_Y_for_burn_z_mix_region

max_X_for_burn_he_mix_region

Even if a region reaches the above temperature to be considered as a z_burn region, only set it as such if the helium mass fraction in all points of the region is below max_Y_for_burn_z_mix_region. Similarly, max_X_for_burn_he_mix_region controls if a region is considered as a he_burn region in terms of the hydrogen mass fraction.

max_Y_for_burn_z_mix_region = 1d-4
max_X_for_burn_he_mix_region = 1d-4

Predictive mixing

Predictive mixing is an approach for expanding convective boundaries until gradr = grada on the convective side of the boundary (as required by the criterion that the convective velocity and luminosity vanish at the boundary). It is discussed in detail in Paxton et al. 2018, ApJ, in press: “Modules for Experiments in Stellar Astrophysics (MESA): Convective boundaries, element diffusion, and massive star explosions”

Predictive mixing is controlled by specifying a set of parameters, which combines matching criteria (determining which boundaries to apply the predictive mixing to) together with values (determining how the predictive mixing should operate at those boundaries). Up to NUM_PREDICTIVE_PARAM_SETS of these parameter sets can be defined (see star_def.inc for value).

predictive_mix

Set to .true. to enable this set of parameters

predictive_mix(1) = .false.

predictive_zone_type

Matching criterion for the type of the convection zone. Possible values are burn_H (hydrogen burning), burn_He (helium burning), burn_Z (metal burning), nonburn (no burning) or any (which matches any type of zone).

predictive_zone_type(1) = ''

predictive_zone_loc

Matching criterion for the location of the convection zone. Possible values are core (the core convection zone), shell (a convective shell), surf (the surface convection zone) or any (which matches any location).

predictive_zone_loc(1) = ''

predictive_bdy_loc

Matching criterion for the location of the convective boundary. Possible values are top (the top of the convection zone), bottom (the bottom of the convection zone) or any (which matches any location).

predictive_bdy_loc(1) = ''

predictive_bdy_q_min

Matching criterion for the minimum fractional mass coordinate of the convective boundary

predictive_bdy_q_min(1) = 0d0

predictive_bdy_q_max

Matching criterion for the maximum fractional mass coordinate of the convective boundary

predictive_bdy_q_max(1) = 1d0

predictive_superad_thresh

Threshold for minimum superadiabaticity in the predictive mixing scheme; boundary expansion stops when gradr/grada-1 drops below this threshold. Default value is usually good for main-sequence evolution; for core He-burning, set to 0.005, 0.01 or larger to prevent splitting of the core convection zone and/or core breathing pulses.

predictive_superad_thresh(1) = 0d0

predictive_avoid_reversal

Species to monitor for reversals in abundance evolution. If this is set to the name of a species, then the predictive mixing scheme will try to avoid causing reversals in the abundance of that species (e.g., changing the abundance evolution from decreasing to increasing). Set to ‘he4’ during core He-burning to prevent splitting of the core convection zone and/or core breathing pulses.

predictive_avoid_reversal(1) = ''

predictive_limit_ingestion

predictive_ingestion_factor

Limit the rate of ingestion of a species, following the prescription given in equation (2) of Constantino, Campbell & Lattanzio (2017, MNRAS, 472, 4900). The control predictive_limit_ingestion specifies which species to limit, and the control predictive_ingestion_factor gives the multiplying factor. Setting this factor to 5/12 is the same as choosing alpha_i = 1 in their equation (2).

predictive_limit_ingestion(1) = ''
predictive_ingestion_factor(1) = 0d0

Convective premixing

Convective premixing is a approach to handling mixing in convection zones that improves upon the predictive mixing scheme described above. Like predictive mixing, it expands convective boundaries until gradr = grada on the convective side of the boundary. Unlike predictive mixing, it directly modifies abundances in the stellar model, via a iterative series of mixings-to-homogeneity over a shifting window of cells. This iterative approach allows convective premixing to build ‘classical’ semiconvection regions, where the abundance gradient is tuned to yield convective neutrality.

NOTE: the history columns that give info on the convective and semi convective boundaries (i.e., mass_conv_core and mass_semiconv_core) do not work with CPM. Instead, one should look at the profiles to see where the boundaries are.

do_conv_premix

Set to .true. to perform convective premixing. Note that this cannot be enabled at the same time as the predictive_mix control

do_conv_premix = .false.

do_premix_heating

if true, calculate heating term associated with changes in internal energy due to any abundance changes from convective premixing, and include this term in the energy equation.

do_premix_heating = .true.

conv_premix_avoid_increase

Attempt to avoid increases in the abundance of species being burned. Sometimes, the convective premixing scheme can cause the abundance of a species being burned (e.g., helium during core helium burning) to increase across a timestep. This typically arises when the scheme mixes a fresh supply of the species into the convection zone where the burning is occurring. Setting the conv_premix_avoid_increase control to .true. will tell the scheme to avoid such outcomes, if possible. In the case of core helium burning, this helps to reduces the incidences of core breathing pulses (although in some situations it doesn’t completely eliminate them).

conv_premix_avoid_increase = .false.

conv_premix_time_factor

Scaling factor for deciding whether a convective boundary has enough time to advance during a timestep. Simple physical arguments suggest that a convective boundary requires a time delta_t ~ delta_r/v_conv to advance a distance delta_r. The convective premixing algorithm keeps a tally of how much time a boundary has spent advancing, and it prevents further advancing if this time would exceed conv_premix_time_factor*dt, where dt is the current timestep. Setting conv_premix_time_factor to a value <= 0 disables this check. STILL UNDER DEVELOPMENT, AND DISABLED BY DEFAULT

conv_premix_time_factor = 0.0

conv_premix_fix_pgas

Flag to decide whether gas pressure is kept constant during premixing (.true.), or instead density is kept constant (.false.). In both cases, temperature is kept constant.

conv_premix_fix_pgas = .true.

conv_premix_dump_snapshots

Flag to write out snapshots of the intermediate stages during the convective premixing iterations. Refer to the dump_snapshot_ routine in star/private/conv_premix.f90 to see what’s written out. Note that this can quickly fill up your disk!

conv_premix_dump_snapshots = .false.

Rayleigh-Taylor Instability

derived from Paul Duffell’s code RT1D.

RTI_smooth_mass

RTI_smooth_iterations

RTI_smooth_fraction

smoothing for dPdr_dRhodr_info done at start of step

RTI_smooth_mass = 0d0
RTI_smooth_iterations = 0
RTI_smooth_fraction = 1d0

alpha_RTI_diffusion_factor

dudt_RTI_diffusion_factor

dedt_RTI_diffusion_factor

dlnddt_RTI_diffusion_factor

composition_RTI_diffusion_factor

max_M_RTI_factors_full_on

min_M_RTI_factors_full_off

alpha_RTI_diffusion_factor = 1d0
dudt_RTI_diffusion_factor = 1d0
dedt_RTI_diffusion_factor = 1d0
dlnddt_RTI_diffusion_factor = 1d0
composition_RTI_diffusion_factor = 1d0
max_M_RTI_factors_full_on = 1d99
min_M_RTI_factors_full_off = 1d99

alpha_RTI_src_max_q

alpha_RTI_src_min_q

option to set alpha_RTI source term to zero when cell q out of bounds. to turn off RTI near surface or center

alpha_RTI_src_max_q = 1d0
alpha_RTI_src_min_q = 0d0

alpha_RTI_src_min_v_div_cs

option to set alpha_RTI source term to zero when v/cs < this min. e.g. to filter out false sources ahead of shock

alpha_RTI_src_min_v_div_cs = 1d0

Radial Stellar Pulsations (RSP)

inspired by Radec Smolec’s Program

must set mass, Teff, L, X, and Z.

RSP_mass = -1
RSP_Teff = -1
RSP_L = -1
RSP_X = -1
RSP_Z = -1

Parameters of the convection model. Note that RSP_alfap, RSP_alfas, RSP_alfac, RSP_alfad and RSP_gammar are expressed in the units of standard values. Standard values are the ones for which static version of the Kuhfuss model reduces to standard MLT. See Table 1 in Smolec & Moskalik (2008) for standard values and the description of the parameters.

RSP_alfa = 1.5d0            ! mixing length; alfa = 0 gives a purely radiative model.
RSP_alfac = 1.0d0           ! convective flux; Lc ~ RSP_alfac
RSP_alfas = 1.0d0           ! turbulent source; Lc ~ 1/ALFAS; PII ~ RSP_alfas
RSP_alfad = 1.0d0           ! turbulent dissipation; damp ~ RSP_alfad
RSP_alfap = 0.0d0           ! turbulent pressure; Pt ~ alfap
RSP_alfat = 0.0d0           ! turbulent flux; Lt ~ RSP_alfat; overshooting.
RSP_alfam = 0.25d0          ! eddy viscosity; Chi & Eq ~ RSP_alfam
RSP_gammar = 0.0d0          ! radiative losses; dampR ~ RSP_gammar

time weighting for end-of-step vs start-of-step values in equations. 1 corresponds to fully implicit scheme - stable, but can have large numerical damping. 0.5 corresponds to trapezoidal rule integration - gives least numerical damping. do not use values less than 0.5. strongly recommend 0.5 for theta and thetat. don’t mess with any of these unless you know what you are doing or like to watch the code crash.

RSP_theta = 0.5d0           ! Pgas and Prad
RSP_thetat = 0.5d0          ! Pturb
RSP_thetae = 0.5d0          ! erad in terms using f_Edd
RSP_thetaq = 1.0d0          ! Pvsc
RSP_thetau = 1.0d0          ! Eq and Uq
RSP_wtr = 0.6667d0          ! Lr
RSP_wtc = 0.6667d0          ! Lc
RSP_wtt = 0.6667d0          ! Lt
RSP_gam = 1.0d0             ! Et src_snk

controls for building the initial model

RSP_nz = 150
RSP_nz_outer = 40
RSP_T_anchor = 11d3
RSP_T_inner = 2d6
RSP_testing = .false.

RSP_dq_1_factor = 2d0
RSP_max_outer_dm_tries = 100
RSP_max_inner_scale_tries = 100
RSP_T_anchor_tolerance = 1d-8

allowed relative difference between T at base of outer region and T_anchor if fail trying to create initial model, try increasing this to 1d-6 or more

RSP_T_inner_tolerance = 1d-8

allowed relative difference between T at inner boundary and T_inner if fail trying to create initial model, try increasing this to 1d-6 or more

RSP_relax_initial_model = .true.
RSP_relax_alfap_before_alfat = .true.
RSP_relax_max_tries = 1000
RSP_relax_dm_tolerance = 1d-6

Initial kick makes use of the scaled linear velocity eigenvector of a given mode or of the linear combination of the eigenvectors for the fundamental mode and first two radial overtones. The surface velocity is set to RSP_kick_vsurf_km_per_sec and the mode content is set by RSP_fraction_1st_overtone and RSP_fraction_2nd_overtone

RSP_kick_vsurf_km_per_sec = 0.1d0
RSP_fraction_1st_overtone = 0d0
RSP_fraction_2nd_overtone = 0d0

fraction from fundamental = 1d0 - (1st + 2nd) Note: This is important for models in which two or more modes are linearly unstable. Appropriate setting may help to arrive at the desired mode, since the final pulsation state may depend on initial conditions set by the three parameters above. Integration of the same model with different initial kicks is a way to study the nonlinear mode selection - for an example see Fig. 1 in Smolec & Moskalik (2010).

random initial velocity profile. added to any kick from eigenvector.

RSP_Avel = 0d0
RSP_Arnd = 0d0

period controls

RSP_target_steps_per_cycle = 600
RSP_min_max_R_for_periods = -1
RSP_min_deltaR_for_periods = -1
RSP_min_PERIOD_div_PERIODLIN = 0.5d0
RSP_mode_for_setting_PERIODLIN = 1
RSP_default_PERIODLIN = 34560

when to stop

RSP_max_num_periods = -1
RSP_GREKM_avg_abs_frac_new = 0.1d0
RSP_GREKM_avg_abs_limit = -1

timestep limiting

RSP_initial_dt_factor = 1d-2

start with smaller timestep to give time for initial model to adjust

RSP_v_div_cs_threshold_for_dt_limit = 0.8d0
RSP_max_dt_times_min_dr_div_cs = 2d0

i.e., make dt <= this times min sound crossing time dr/cs only considering cells with abs(v)/cs > threshold

RSP_max_dt_times_min_rad_diff_time = -1d0

make dt <= min time for radiative diffusion for RHD

RSP_max_dt = -1
RSP_report_limit_dt = .false.

artificial viscosity controls for the equations see: Appendix C in Stellingwerf (1975). In principle, for not too-non-adiabatic convective models artificial viscosity is not needed or should be very small. Hence a large cut-off parameter below (in purely radiative models the default value for cut-off was 0.01)

RSP_cq = 4.0d0
RSP_zsh = 0.1d0

zsh > 0 delays onset of artificial viscosity can eliminate most/all interior dissipation while still providing for extreme cases. using this parameter the dependence of limiting amplitude on cq is very weak. for Tscharnuter & Winkler form of artificial viscosity

RSP_Qvisc_linear = 0d0
RSP_Qvisc_quadratic = 0d0

as described in section 4.2 of mesa3, 2015. RSP_Qvisc_linear is analogous to shock_spread_linear RSP_Qvisc_quadratic is analogous to shock_spread_quadratic if switch to this form, set RSP_cq = 0 to shut off the Neumann & Richtmyer form. note that this form also uses RSP_zsh to delay onset of artificial viscosity

surface pressure. provides outer boundary condition for momentum equation.

RSP_use_Prad_for_Psurf = .false.
RSP_use_atm_grey_with_kap_for_Psurf = .false.
RSP_tau_surf_for_atm_grey_with_kap = 3d-3
RSP_fixed_Psurf = .true.
RSP_Psurf = 0d0
set_RSP_Psurf_to_multiple_of_initial_P1 = -1

set RSP_Psurf to this times initial surface cell pressure

RSP_surface_tau = 0.001d0

solver controls

RSP_tol_max_corr = 1d-8
RSP_tol_max_resid = 1d-6
RSP_max_iters_per_try = 100
RSP_max_retries_per_step = 50
RSP_report_undercorrections = .false.
RSP_nz_div_IBOTOM = 30d0
RSP_min_tau_for_turbulent_flux = 2d2

output data for work integrals during a particular period

RSP_work_period = -1
RSP_work_filename = 'work.data'

output data for 3d map. format same as for gnuplot pm3d

RSP_write_map = .false.
RSP_map_columns_filename = 'map_columns.list'

items listed in your map columns must also appear in your profile columns

RSP_map_filename = 'map.data'
RSP_map_first_period = -1
RSP_map_last_period = -1
RSP_map_zone_interval = 2
RSP_map_history_filename = 'map_history.data'

rsp hooks

use_other_RSP_linear_analysis = .false.
use_other_RSP_build_model = .false.

for special tests can set ALFA = 0 for pure radiative with no turbulence or convection. can set zero_gravity = .true. can set opacity to be constant times density.

RSP_kap_density_factor = -1

else set opacity to this times density

rsp misc

RSP_efl0 = 1.0d2
RSP_nmodes = 3
RSP_trace_RSP_build_model = .false.

use_RSP_new_start_scheme = .false.

RSP_Qvisc_linear_static = 0d0

RSP_relax_adjust_inner_mass_distribution = .true.

RSP_do_check_omega = .true.

RSP_report_check_omega_changes = .false.

RSP_hydro_only = .false.

this does not work with the standard build model, so requires use_other_RSP_build_model

mixing misc

such as smoothing and editing of diffusion coefficients

mix_factor

Mixing coefficients are multiplied by this factor. The mix_factor is applied in subroutine get_convection_sigmas in star/private/mix_info.f90 – the lagrangian diffusion coefficient sigma(k) at cell boundary k is set to mix_factor*D*(4*pi*r(k)^2*rho_face(k))^2. Note that the value of D is not changed – it is just used as a term in calculating sigma.

mix_factor = 1

max_conv_vel_div_csound

convective velocities are limited to local sound speed times this factor.

max_conv_vel_div_csound = 1d99

max_conv_vel_div_csound_maxq

only consider max_conv_vel_div_csound from center out to this location

max_conv_vel_div_csound_maxq = -1

max_v_for_convection

disable convection for locations with v > than this limit. In km/s.

max_v_for_convection = 1d99

max_q_for_convection_with_hydro_on

disable convection for locations with q > than this limit when either v_flag or u_flag are true.

max_q_for_convection_with_hydro_on = 1d99

max_v_div_cs_for_convection

disable convection for locations with abs(v)/cs > this limit

max_v_div_cs_for_convection = 1d99

max_abs_du_div_cs_for_convection

main purpose is to force radiative in shock face

max_abs_du_div_cs_for_convection = 0.03d0

prune_bad_cz_min_Hp_height

Lower limit on radial extent of cz (<= 0 to disable). In units of average pressure scale height at top and bottom of region. Remove tiny convection zones unless have strong nuclear burning This allows emergence of very small cz at site of he core flash, for example. i.e., remove if size < prune_bad_cz_min_Hp_height .and. max_log_eps < prune_bad_cz_min_log_eps_nuc.

prune_bad_cz_min_Hp_height = 0

prune_bad_cz_min_log_eps_nuc

Lower limit on max log eps nuc in cz. remove if size < prune_bad_cz_min_Hp_height .and. max_log_eps < prune_bad_cz_min_log_eps_nuc.

prune_bad_cz_min_log_eps_nuc = -99

redo_conv_for_dr_lt_mixing_length

Check for small convection zones with total height less than mixing length and redo with reduced mixing_length_alpha to make mixing_length <= dr.

redo_conv_for_dr_lt_mixing_length = .false.

smooth_convective_bdy has been deleted.

remove_mixing_glitches

If true, then okay to remove gaps and singletons.

remove_mixing_glitches = .true.

glitches

The following controls are for different kinds of “glitches” that can be removed.

okay_to_remove_mixing_singleton

If true, remove singletons.

okay_to_remove_mixing_singleton = .true.

clip_D_limit

Zero mixing diffusion coeffs that are smaller than this.

clip_D_limit = 0

min_convective_gap

Close gap between convective regions if smaller than this (< 0 means skip this). Gap measured radially in units of pressure scale height.

min_convective_gap = -1

min_thermohaline_gap

Close gap between thermohaline mixing regions if smaller than this (< 0 means skip this). Gap measured radially in units of pressure scale height.

min_thermohaline_gap = -1

min_thermohaline_dropout

max_dropout_gradL_sub_grada

If find radiative region embedded in thermohaline, and max(gradL - grada) in region is everywhere < max_dropout_gradL_sub_grada and region height is < min_thermohaline_dropout then convert the region to thermohaline. min_thermohaline_dropout <= 0 disables.

min_thermohaline_dropout = -1
max_dropout_gradL_sub_grada = 1d-3

min_semiconvection_gap

Close gap between semiconvective mixing regions if smaller than this (< 0 means skip this). Gap measured radially in units of pressure scale height.

min_semiconvection_gap = -1

remove_embedded_semiconvection

If have a semiconvection region bounded on each side by convection, convert it to be convective too.

remove_embedded_semiconvection = .false.

recalc_mix_info_after_evolve

Re-evaluate mixing info after each evolve step. This is helpful if you want the profiles to reflect the mixing params after the step; otherwise, they give the mixing info from the start of the step (i.e., one step out-of-date)

recalc_mix_info_after_evolve = .false.

set_min_D_mix

mass_lower_limit_for_min_D_mix

mass_upper_limit_for_min_D_mix

min_D_mix

D_mix will be at least this large if set_min_D_mix is true. doesn’t apply for mass < lower limit or mass > upper limit.

set_min_D_mix = .false.
mass_lower_limit_for_min_D_mix = 0d0
mass_upper_limit_for_min_D_mix = 1d99
min_D_mix = 1d3

set_min_D_mix_in_H_He

min_D_mix_in_H_He

D_mix will be at least this large in regions where max mass fractions of H and He add to more that 0.5 if set_min_D_mix_in_H_He is true.

set_min_D_mix_in_H_He = .false.
min_D_mix_in_H_He = 1d3

set_min_D_mix_below_Tmax

min_D_mix_below_Tmax

D_mix will be at least this large for cells below location of max temperature if set_min_D_mix_below_Tmax is true.

set_min_D_mix_below_Tmax = .false.
min_D_mix_below_Tmax = 1d3

min_center_Ye_for_min_D_mix

min_D_mix is only used when center_ye >= this i.e., when center_ye drops below this, min_D_mix = 0.

min_center_Ye_for_min_D_mix = 0.47d0

smooth_outer_xa_big

smooth_outer_xa_small

Soften composition jumps in outer layers. If smooth_outer_xa_big and smooth_outer_xa_small are bigger than 0, then starting from the outermost grid point, homogeneously mix a region of size smooth_outer_xa_small (in solar masses), and proceed inwards, linearly reducing the size of the homogeneously mixed region in such a way that it becomes zero. After going smooth_outer_xa_big solar masses in. In this way, the outer smooth_outer_xa_big solar masses are “cleaned” of composition jumps.

smooth_outer_xa_big = -1d0
smooth_outer_xa_small = -1d0

rotation controls

In the following “am” stands for “angular momentum”.

the mesa implementation of rotation closely follows these papers:

• Heger, Langer, & Woosley, ApJ, 528, 368. 2000

• Heger, Woosley, & Spruit, ApJ, 626, 350. 2005

• D_DSI = dynamical shear instability

• D_SH = Solberg-Hoiland

• D_SSI = secular shear instability

• D_ES = Eddington-Sweet circulation

• D_GSF = Goldreich-Schubert-Fricke

• D_ST = Spruit-Tayler dynamo

skip_rotation_in_convection_zones

if true, then set rotational diffusion coefficients to 0 in convective regions. This applies both for material mixing and diffusion of angular momentum.

skip_rotation_in_convection_zones = .false.

am_D_mix_factor

Rotation and mixing of material. D_mix = diffusion coefficient for mixing of material. It is sum of non-rotational and rotational components. The rotational part is multiplied by this factor.

D_mix = D_mix_non_rotation + f*am_D_mix_factor*(
    D_DSI_factor * D_DSI +
    D_SH_factor  * D_SH +
    D_SSI_factor * D_SSI +
    D_ES_factor  * D_ES +
    D_GSF_factor * D_GSF +
    D_ST_factor  * D_ST)

f = 1  when logT <= D_mix_rotation_max_logT_full_on = full_on
  = 0  when logT >= D_mix_rotation_min_logT_full_on = full_off
  = (log(T)-full_on)/(full_off-full_on) else

note that for regions with brunt N^2 < 0, we set Richardson number to 1 which is > Ri_critical and therefore turns off DSI and SSI

according to Heger et al 2000 : 1/30d0 by default : 0

am_D_mix_factor = 0

am_nu_factor

am_nu_non_rotation_factor

diffusion of angular momentum

am_nu = diffusion coefficient for angular momentum

am_nu_non_rot = am_nu_factor*am_nu_non_rotation_factor*D_mix_non_rotation
am_nu_rot = am_nu_factor*(
    am_nu_visc_factor* D_visc +
    am_nu_DSI_factor * D_DSI +
    am_nu_SH_factor  * D_SH +
    am_nu_SSI_factor * D_SSI +
    am_nu_ES_factor  * D_ES +
    am_nu_GSF_factor * D_GSF +
    am_nu_ST_factor  * nu_ST)
am_nu = am_nu_non_rot + am_nu_rot

Note that for regions with brunt N^2 < 0, we set Richardson number to 1 which is > Ri_critical and therefore turns off DSI and SSI.

see also star_job controls for am_nu_rot_flag

am_nu_factor = 1
am_nu_non_rotation_factor = 1

am_nu_DSI_factor

< 0 means use D_DSI_factor

am_nu_DSI_factor = -1

am_nu_SSI_factor

< 0 means use D_SSI_factor

am_nu_SSI_factor = -1

am_nu_SH_factor

< 0 means use D_SH_factor

am_nu_SH_factor = -1

am_nu_ES_factor

< 0 means use D_ES_factor

am_nu_ES_factor = -1

am_nu_GSF_factor

< 0 means use D_GSF_factor

am_nu_GSF_factor = -1

am_nu_ST_factor

< 0 means use D_ST_factor

am_nu_ST_factor = -1

am_nu_visc_factor

< 0 means use D_visc_factor. By default = 1 to mix angular momentum.

am_nu_visc_factor = 1

am_nu_omega_rot_factor

am_nu_omega_non_rot_factor

dj/dt = d/dm((4 pi r^2 rho)^2*(am_nu_omega*i_rot*domega/dm + am_nu_j*dj/dm)) am_nu_omega = am_nu_omega_non_rot_factor*am_nu_non_rot + am_nu_omega_rot_factor*am_nu_rot

am_nu_omega_rot_factor = 1
am_nu_omega_non_rot_factor = 1

am_nu_j_rot_factor

am_nu_j_non_rot_factor

dj/dt = d/dm((4 pi r^2 rho)^2*(am_nu_omega*i_rot*domega/dm + am_nu_j*dj/dm)) am_nu_j = am_nu_j_non_rot_factor*am_nu_non_rot + am_nu_j_rot_factor*am_nu_rot

am_nu_j_rot_factor = 0
am_nu_j_non_rot_factor = 0

set_uniform_am_nu_non_rot

uniform_am_nu_non_rot

You can specify a uniform value for am_nu_non_rot by setting this flag true. A large uniform am_nu will produce a uniform omega.

set_uniform_am_nu_non_rot = .false.
uniform_am_nu_non_rot = 1d20

set_min_am_nu_non_rot

min_am_nu_non_rot

You can also specify a minimum am_nu_non_rot. am_nu will be at least this large.

set_min_am_nu_non_rot = .false.
min_am_nu_non_rot = 1d8

min_center_Ye_for_min_am_nu_non_rot

min_am_nu_non_rot is only used when center Ye >= this.

min_center_Ye_for_min_am_nu_non_rot = 0.47d0

Each rotationally induced diffusion coefficient has a factor that lets you control it. Value of 1 gives normal strength; value of 0 turns it off.

Note that for regions with brunt N^2 < 0, we set Richardson number to 1, which is > Ri_critical and therefore turns off DSI and SSI.

D_DSI_factor = 0
D_SH_factor = 0
D_SSI_factor = 0
D_ES_factor = 0
D_GSF_factor = 0
D_ST_factor = 0

D_visc_factor

Kinematic shear viscosity. Should be = 0 because viscosity doesn’t mix chemical elements.

D_visc_factor = 0

am_gradmu_factor

Sensitivity to composition gradients. In calculation of rotational induced mixing, grad_mu is multiplied by am_gradmu_factor. Value from from Heger et al 2000.

am_gradmu_factor = 0.05d0

Spatial smoothing is used in calculations of diffusion coefficients. These control the smoothing window widths (number of cells on each side).

smooth_D_DSI = 0
smooth_D_SH = 0
smooth_D_SSI = 0
smooth_D_ES = 0
smooth_D_GSF = 0
smooth_D_ST = 0
smooth_nu_ST = 0
smooth_D_omega = 0
smooth_am_nu_rot = 0

ST_angsmt

ST_angsml

Temporal smoothing of ST coefficients. See rotation_mix_info.f90 for details

ST_angsmt = 0.2d0
ST_angsml = 1d-3

simple_i_rot_flag

If true, i_rot = (2/3)*r^2. If false, use slightly more complex expression that takes into account finite shell thickness. In practice, there doesn’t seem to be a significant difference.

simple_i_rot_flag = .false.

do_adjust_J_lost

adjust_J_fraction

adjust angular momentum With do_adjust_J_lost = .false., the angular momentum removed via winds from the star corresponds to that contained in the removed layers. However, since j_rot can increase steeply in the very outer layers, very small steps are required to obtain a convergent solution. To avoid this, the do_adjust_J_lost option adjusts the angular momentum content of layers below those removed, such that

actual_J_lost = &
   adjust_J_fraction*mass_lost*s% j_rot_surf + &
   (1d0 - adjust_J_fraction)*s% angular_momentum_removed

where s% angular_momentum_removed is the angular momentum contained in the removed layers of the star in that step. Note that s% angular_momentum_removed is set to actual_J_lost after this.

The region from which angular momentum is removed is chosen such that at its bottom q<min_q_for_adjust_J_lost, it contains at least min_J_div_delta_J times the angular momentum that needs to be accounted for. Angular momentum in these regions is adjusted in such a way that no artificial shear is produced at the inner boundary.

This can also be used to model mass loss mechanisms that remove more angular momentum than mass_lost*s% j_rot_surf, for instance magnetic braking or wind mass loss. In that case, you can use the use_other_j_for_adjust_J_lost option to specify a specific angular momentum of removed material different from j_rot_surf

In order to prevent the algorithm from digging to deep to adjust J, there is a timestep limit adjust_J_q_limit

do_adjust_J_lost = .true.
adjust_J_fraction = 1d0
min_q_for_adjust_J_lost = 0.995d0
min_J_div_delta_J = 3d0

premix_omega

if premix_omega is true, then do 1/2 of the transport of angular momentum before updating the structure and 1/2 after. otherwise, do all of the transport after updating the structure. RECOMMENDED to turn it on when modelling an accreting star or when using do_adjust_J_lost.

premix_omega = .true.

angular_momentum_error_warn

angular_momentum_error_stop

if the relative change in total angular momentum exceeds these values, then a warning is given on the terminal output, or the simulation is stopped altogether. Not applied when using other_torque routines or for binaries.

angular_momentum_error_warn = 5d-6
angular_momentum_error_retry = 1d-6

recalc_mixing_info_each_substep

if recalc_mixing_info_each_substep is true, then recalculate the omega mixing coefficients after each substep of the solve omega mix process.

recalc_mixing_info_each_substep = .false.

w_div_wcrit_max

When fitted_fp_ft_i_rot = .true., limit fp and ft to their values at this w_div_wcrit

w_div_wcrit_max = 0.89d0

w_div_wcrit_max2

When w_div_wc_flag is true, rather than a hard limit on w_div_wcrit we use two limiting values w_div_wcrit_max < w_div_wcrit_max2 to provide a smooth transition. Nothing is done when w_div_wc < w_div_wcrit_max, if w_div_wcrit_max < w_div_wc < w_div_wcrit_max2, we apply a sigmoid, and in the limit of j_rot -> infinity, the resulting w_div_wc will match w_div_wcrit_max2 (being on the top of the sigmoid)

w_div_wcrit_max2 = 0.90d0

D_mix_rotation_max_logT_full_on

Use rotational components of D_mix for locations where logT <= this. For numerical stability, turn off rotational part of D_mix at very high T.

D_mix_rotation_max_logT_full_on = 9.4d0

D_mix_rotation_min_logT_full_off

Drop rotational components of D_mix for locations where logT >= this. For numerical stability, turn off rotational part of D_mix at very high T.

D_mix_rotation_min_logT_full_off = 9.5d0

D_mix_rotation_min_tau_full_off

Drop rotational components of D_mix for locations where tau <= this. For numerical stability, turn off rotational part of D_mix at very low tau.

D_mix_rotation_min_tau_full_off = 0d0

D_mix_rotation_max_tau_full_on

Use rotational components of D_mix for locations where tau >= this. For numerical stability, turn off rotational part of D_mix at very low tau.

D_mix_rotation_min_tau_full_on = 0d0

D_omega_max_replacement_fraction

D_omega_growth_rate

D_omega_mixing_rate

D_omega_mixing_across_convection_boundary (previously called D_omega_mixing_in_convection_regions)

D_omega_mixing_rate = 1d0
D_omega_mixing_across_convection_boundary = .false.
max_q_for_D_omega_zero_in_convection_region = 0.8d0

nu_omega_max_replacement_fraction

nu_omega_growth_rate

nu_omega_mixing_rate

nu_omega_mixing_across_convection_boundary

nu_omega_mixing_rate = 1d0
nu_omega_mixing_across_convection_boundary = .false.
max_q_for_nu_omega_zero_in_convection_region = 0.8d0

atmosphere boundary conditions

atm_option

Controls how the surface temperature Tsurf and pressure Psurf are evaluated when setting up outer boundary conditions. We caution that the use of 'fixed_' atmosphere options might conflict with mlt_option = TDC.

• 'T_tau': set Tsurf and Psurf by solving for the atmosphere structure given a T(tau) relation. The choice of relation is set by the atm_T_tau_relation control. See also the atm_T_tau_opacity, atm_T_tau_errtol, atm_T_tau_max_tries and atm_T_tau_max_steps controls.

• 'table': set Tsurf and Psurf by interpolating in pre-calculated tables based on model atmospheres. The choice of table is set by the atm_table control. Requires tau_factor = 1, as surface of the model must always attach at the base of the tables, so there is no flexibility to move model surface inward or outward. Note that tau_base = tau_surf is the location at which the model attaches to the table BCs, and there is no particular location identified as the photosphere, so we fall back to the surface values of L, R, and m to calculate quantities such as Teff and log_g. This is consistent with the assumptions used for table construction: geometrically thin atmospheres with constant flux.

• 'irradiated_grey': set Tsurf by solving for the atmosphere structure given the irradiated-grey T(tau) relation of Guillot, T, and Havel, M., A&A 527, A20 (2011). See also the atm_irradiated_opacity, atm_irradiated_errtol, atm_irradiated_T_eq, atm_irradiated_T_eq, atm_irradiated_kap_v, atm_irradiated_kap_v_div_kap_th, atm_irradiated_P_surf and atm_irradiated_max_tries controls.

• 'fixed_Teff' :

  set Tsurf from Eddington T(tau) relation for current surface tau and Teff = atm_fixed_Teff. set Psurf = Radiation_Pressure(Tsurf)

• 'fixed_Tsurf' :

  get value of Tsurf from control parameter atm_fixed_Tsurf. set Teff from Eddington T(tau) relation for given Tsurf and tau=2/3 set Psurf = Radiation_Pressure(Tsurf)

• 'fixed_Psurf' :

  get value of Psurf from control parameter atm_fixed_Psurf. set Tsurf from L and R using L = 4*pi*R^2*boltz_sigma*T^4. set Teff using Eddington T(tau) relation for tau=2/3 and T=Tsurf.

• 'fixed_Psurf_and_Tsurf' :

  get value of Psurf from control parameter atm_fixed_Psurf. get value of Tsurf from control parameter atm_fixed_Tsurf. see the conductive_flame test_suite for an example of this boundary condition implemented via the other_surface_PT hook.

atm_option = 'T_tau'

atm_off_table_option

If have selected 'table' for atm_option, fallback to using this if the args are off the table. Possible choices are 'T_tau' or blank (in which case the code will halt when it encounters an off-table arg)

atm_off_table_option = 'T_tau'

atm_fixed_Teff

Set this when using atm_option = 'fixed_Teff'

atm_fixed_Teff = 0

atm_fixed_Tsurf

Set this when using atm_option = 'fixed_Tsurf'

atm_fixed_Tsurf = 0

atm_fixed_Psurf

Set this when using atm_option = 'fixed_Psurf'

atm_fixed_Psurf = -1

Pextra_factor

Parameter for extra pressure in surface boundary conditions. Pressure at optical depth tau is calculated as P = tau*g/kap*(1 + Pextra) Pextra takes into account nonzero radiation pressure at tau=0. The equation for Pextra includes Pextra_factor

Pextra = Pextra_factor*(kap/tau)*(L/M)/(6d0*pi*clight*cgrav)

For certain situations such super eddington L, you may need to increase Pextra to help convergence. e.g. try Pextra_factor = 2

Note that Pextra_factor is only applied when atm_option = 'T_tau' and atm_T_tau_opacity = 'fixed' or ‘iterated'.

Pextra_factor = 1

atm_T_tau_relation

The T(tau) relation to use when atm_option = 'T_tau'

• 'Eddington': use the grey Eddington T(tau) relation.

• 'solar_Hopf': use a grey T(tau) relation with an approximate Hopf function tuned to solar data. See Paper II, Sec. A.5. Equivalent to the fit given by Sonoi et al. (2019, A&A, 621, 84) to the Vernazza et al. (1981) VAL-C model.

• 'Krishna_Swamy': use the grey T(tau) relation described by K.S. Krishna-Swamy, ApJ 145, 174–194 (1966).

• 'Trampedach_solar': use the analytic fit by Ball (2021, RNAAS 5, 7) to the Hopf function for the solar simulation by Trampedach et al. (2014, MNRAS 442, 805–820)

atm_T_tau_relation = 'Eddington'

atm_T_tau_opacity

Controls how opacities are calculated throughout the atmosphere when atm_option = 'T_tau'

• 'fixed': use a uniform opacity, fixed to the opacity of the outermost cell of the interior model

• 'iterated': use a uniform opacity, iterated to be consistent with the final Tsurf and Psurf at the base of the atmosphere.

• 'varying': use a varying opacity consistent with the local T and P throughout the atmosphere. Involves numerical integration of the hydrostatic equilibrium equation.

atm_T_tau_opacity = 'fixed'

atm_T_tau_errtol

Error tolerance for iterations and integrations when atm_option = 'T_tau' and atm_T_tau_opacity = 'iterated' or 'varying'.

atm_T_tau_errtol = 1d-7

atm_T_tau_max_iters

Maximum number of iterations for the opacity when atm_option = 'T_tau' and atm_T_tau_opacity = 'iterated'.

atm_T_tau_max_iters = 50

atm_T_tau_max_steps

Maximum number of steps for integrating the hydrostatic equilibrium equation when atm_option = 'T_tau' and atm_T_tau_opacity = 'varying'.

atm_T_tau_max_steps = 500

atm_table

Determines which table Tsurf and Psurf are interpolated in

• 'tau_100', 'tau_10', 'tau_1', 'tau_1m1': use model atmosphere tables for Pgas and T at tau=100, 10, 1 or 0.1, respectively; solar Z only, as described in MESA Paper I (Paxton et al. 2011), Sec. 5.3. these tables are primarily for the evolution of low-mass stars, brown dwarfs, and giant planets. They are constructed from Castelli & Kurucz (2003) for Teff > 3000 K and the COND model atmospheres (Allard et al. 2001) for Teff < 3000 K. where no published results are available, the table has been filled in using integration of the Eddington T(tau) relation

• 'photosphere': use model atmosphere tables for photosphere; range of Z’s, as described in MESA Paper I (Paxton et al. 2011), Sec. 5.3. the tables cover log(Z/Zsun) from -4 to 0.5 for a GN93 solar mixture, and span logg = -0.5 to 5.5 in steps of 0.5 dex and Teff = 2000 to 50 000 K in steps of 250 K. they are constructed, in order of precedence, using the PHOENIX model atmospheres (Hauschildt et al. 1999a,b) and the models by Castelli & Kurucz (2003). where neither is available, an entry is generated by integrating the Eddington T(tau) relation

• 'WD_tau_25': hydrogen atmosphere tables for cool white dwarfs giving Pgas and T at log10(tau) = 1.4 (tau = 25.11886) Teff goes from 40,000 K down to 2,000K with step of 100 K Log10(g) goes from 9.5 down to 5.5 with step of 0.1. R.D. Rohrmann, L.G. Althaus, and S.O. Kepler, Lyman α wing absorption in cool white dwarf stars, Mon. Not. R. Astron. Soc. 411, 781–791 (2011)

• 'DB_WD_tau_25': helium dominated (log(H/He)=-5.0) atmosphere tables for DB white dwarfs, provided by Odette Toloza and Detlev Koester. 5000K < Teff < 40000K

atm_table = 'tau_100'

atm_irradiated_opacity

Controls how thermal opacities are calculated throughout the atmosphere when atm_option = 'irradiated_grey'

• 'fixed': use a uniform opacity, fixed to the opacity of the outermost cell of the interior model.

• 'iterated': use a uniform opacity, iterated to be consistent with the final Tsurf and Psurf at the base of the atmosphere.

atm_irradiated_opacity = 'fixed'

atm_irradiated_errtol

Error tolerance for iterations when atm_option = 'irradiated_grey' and atm_irradiated_opacity = 'iterated'.

atm_irradiated_errtol = 1d-7

atm_irradiated_max_iters

Maximum number of iterations for the opacity when atm_option = 'irradiated_grey' and atm_irradiated_opacity = 'iterated'.

atm_irradiated_max_iters = 50

atm_irradiated_T_eq

Equilibrium temperature based on irradiation.

irrad_flux = Lstar/(4*pi*orbit**2)

• Area of planet in plane perpendicular to irrad_flux = pi*Rplanet**2.

• Stellar luminosity received by planet = irrad_flux*area.

• This luminosity determines T_eq: T_eq**4 = irrad_flux/(4*sigma).

atm_irradiated_T_eq = 100

atm_irradiated_kap_v_div_kap_th

atm_irradiated_kap_v

The T(tau) relation when atm_option = 'irradiated_grey' depends on the ratio kap_v/kap_th where kap_v is the planet atmosphere opacity for stellar irradiation, and kap_th is the thermal opacity for the internally produced radiation. There are two ways to calculate the ratio:

• if atm_irradiated_kap_v_div_kap_th > 0, then use it for kap_v/kap_th

• if atm_irradiated_kap_v_div_kap_th == 0, then use atm_irradiated_kap_v to set kap_v, and then evaluate the ratio using kap_th

atm_irradiated_kap_v_div_kap_th = 0
atm_irradiated_kap_v = 4d-3

atm_irradiated_P_surf

Surface pressure when atm_option = 'irradiated_grey'; default is 1 bar in cgs units.

atm_irradiated_P_surf = 1d6

use_compression_outer_BC

gradient of compression vanishes at surface

see Grott, Chernigovski, Glatzel, 2005. d_dm(d_dm(r^2*v)) = 0 at surface by continuity, this is d_dm(d_dt(1/rho)) = 0 at surface finite volume form is (1/rho(1) - 1/rho_start(1)) = (1/rho(2) - 1/rho_start(2)) this BC determines the density for surface cell.

use_compression_outer_BC = .false.

use_momentum_outer_BC

use P_surf from atm to set pressure gradient at surface in momentum equation calculate v(1) based on pressure difference P_surf - P(1)

use_momentum_outer_BC = .false.

use_zero_Pgas_outer_BC

use Psurf = Radiation_Pressure(T_start(1))

use_zero_Pgas_outer_BC = .false.

use_fixed_vsurf_outer_BC

fixed_vsurf

v at outer boundary of model is set to be fixed_vsurf

use_fixed_vsurf_outer_BC = .false.
fixed_vsurf = 0

use_fixed_Psurf_outer_BC

fixed_Psurf

P at outer boundary of model is set to be fixed_Psurf

use_fixed_Psurf_outer_BC = .false.
fixed_Psurf = 0

Tsurf_factor

used when use_momentum_outer_BC T_surf is set to Tsurf_factor*T_black_body(L_surf,R_surf)

Tsurf_factor = 1

irradiation_flux

column_depth_for_irradiation

irradiation_flux = 0
column_depth_for_irradiation = -1

atm_build_tau_outer

atm_build_dlogtau

atm_build_errtol

Parameters controlling atmosphere structure building. MESA can evaluate the spatial structure of the atmosphere for the following atm_option choice:

• 'T_tau'

The atmosphere structure data are appended to the interior model when add_atmosphere_to_pulsation = .true.. They do not affect the surface boundary conditions applied to the interior model.

atm_build_tau_outer specifies the outermost optical depth to include in the atmosphere; atm_build_dlntau specifies the spacing of atmosphere points in (base-10) logarithmic optical depth; and atm_build_errtol specifies the error tolerance for evaluating the structure.

atm_build_tau_outer = 1d-3
atm_build_dlogtau = 0.01
atm_build_errtol = 1d-8

use_T_tau_gradr_factor

If .true., modify the radiative gradient so that the temperature profile of the optically thin layers follow the T(τ) relation chosen by atm_T_tau_relation.

use_T_tau_gradr_factor = .false.

starspots

do_starspots

If .true., switch on impedance of the surface flux due to magnetic pressure from starspots, parameterized in the style of an atmospheric boundary modification. First described by Somers et al. (2015; ApJ). Detailed discussion of this functionality can be found in MESA V.

do_starspots = .false.

fspot

Filling Factor of starspots. Valid values between 0.0 and 1.0 (no spots to 100% coverage)

fspot = 0d0

xspot

Temperature contrast between the spotted and unspotted regions. Valid values are between 1.0 (no contribution from magnetic pressure) and 0.5 (half of the total pressure is due to magnetic pressure)

xspot = 1d0

mass gain or loss

mass_change

Rate of accretion (Msun/year). Negative for mass loss. This only applies when the wind_scheme = ''.

mass_change = 0d0

mdot_omega_power

Enhanced mass loss due to rotation as in Heger, Langer, and Woosley, 2000, ApJ, 528:368-396.

Mdot = Mdot_no_rotation/(1 - Osurf/Osurf_crit)^mdot_omega_power

where

Osurf = angular velocity at surface Osurf_crit^2 = (1 - Gamma_edd)*G*M/R^3 Gamma_edd = kappa*L/(4 pi c G M), Eddington factor

Typical value for mdot_omega_power = 0.43.

Set to 0 to disable this feature.

mdot_omega_power = 0.43d0

max_rotational_mdot_boost

This limits the rotational boost.

max_rotational_mdot_boost = 1d4

max_mdot_jump_for_rotation

Don’t increase prev mdot by more that this.

max_mdot_jump_for_rotation = 2

lim_trace_rotational_mdot_boost

Output to terminal if boost > this.

lim_trace_rotational_mdot_boost = 1d99

rotational_mdot_boost_fac

Increase mdot.

rotational_mdot_boost_fac = 1d5

rotational_mdot_kh_fac

Kelvin-helmholtz boost.

rotational_mdot_kh_fac = 0.3d0

surf_avg_tau_min

Use mass avg starting from this optical depth.

surf_avg_tau_min = 1

surf_avg_tau

Use mass avg down to this optical depth.

surf_avg_tau = 100

hot_wind_scheme

cool_wind_RGB_scheme

cool_wind_AGB_scheme

This section replaces the old “RGB_wind_scheme” and “AGB_wind_scheme” with temperature-dependent hot_wind and cool_wind. You can still use the RGB and AGB wind scheme as before, the functionality remains.

Now you can also select a hot wind scheme that takes effect above some temperature, set by hot_wind_full_on_T. Similarly, the cool wind scheme has temperature controls that set the temperature below which they are relevant (cool_wind_full_on_T).

As before, an empty string ‘’ means no wind.

The wind “eta” values, which are constant scaling factors, have all renamed *_wind_eta -> *_scaling_factor.

Here is an example of how to translate an existing inlist from the old style to the new:

Before	After
RGB_wind_scheme = ‘Reimers’ Reimers_wind_eta = 0.1 AGB_wind_scheme = ‘Blocker’ Blocker_wind_eta = 0.5 RGB_to_AGB_wind_switch = 1d-4	cool_wind_RGB_scheme = ‘Reimers’ Reimers_scaling_factor = 0.1 cool_wind_AGB_scheme = ‘Blocker’ Blocker_scaling_factor = 0.5 RGB_to_AGB_wind_switch = 1d-4 ! only use the cool_wind_scheme cool_wind_full_on_T = 1d10 !K hot_wind_full_on_T = 1.1d10 !K hot_wind_scheme = ‘’

suggested hot and cool wind schemes follow but any valid wind option will work for either hot or cool.

Empty string means no wind

Suggested hot wind option:

• ‘Vink’

• ‘Bjorklund’

Suggested cool wind options:

• ‘Reimers’

• ‘Blöcker’

• ‘de Jager’

• ‘van Loon’

• ‘Nieuwenhuijzen’

For now the ‘Dutch’ scheme can be used in either capacity.

NOTE: for schemes that scale with metallicitity, we use Zbase rather than Z (as long as Zbase > 0). This is because wind mass loss rate is primarily determined by iron opacity, which is unlikely to change during the evolution.

hot_wind_scheme = ''
cool_wind_RGB_scheme = ''
cool_wind_AGB_scheme = ''

cool_wind_full_on_T

hot_wind_full_on_T

NOTE: hot_wind_full_on_T was previously called ‘cool_wind_full_off_T’

use only cool wind schemes for T_phot < cool_wind_full_on_T use only hot wind schemes for T_phot > hot_wind_full_on_T if cool_wind_full_on_T /= hot_wind_full_on_T then ramp between these limits requires hot_wind_full_on_T > cool_wind_full_on_T

cool_wind_full_on_T = 0.8d4
hot_wind_full_on_T = 1.2d4

RGB_to_AGB_wind_switch

If center hydrogen abundance is < 0.01 and center helium abundance by mass is less than RGB_to_AGB_wind_switch, then system will use AGB_wind_scheme rather than RGB_wind_scheme.

RGB_to_AGB_wind_switch = 1d-4

The code will automatically choose between an RGB wind and an AGB wind. The following names for the different schemes are recognized:

• ‘Reimers’

• ‘Blocker’

• ‘de Jager’

• ‘van Loon’

• ‘Nieuwenhuijzen’

• ‘Vink’

• ‘Dutch’

• ‘Bjorklund’

• ‘other’ — for wind options implemented using other_wind hook

Reimers_scaling_factor

Reimers mass loss for red giants.

D. Reimers “Problems in Stellar Atmospheres and Envelopes” Baschek, Kegel, Traving (eds), Springer, Berlin, 1975, p. 229.

Parameter for mass loss by Reimers wind prescription. Reimers mdot is eta*4d-13*L*R/M (Msun/year), with L, R, and M in solar units. Typical value is 0.5.

Reimers_scaling_factor = 0

Blocker_scaling_factor = 0

Blocker’s mass loss for AGB stars.

T. Blocker “Stellar evolution of low and intermediate-mass stars” A&A 297, 727-738 (1995).

Parameter for mass loss by Blocker’s wind prescription. Blocker mdot is eta*4.83d-9*M**-2.1*L**2.7*4d-13*L*R/M (Msun/year), with L, R, and M in solar units. Typical value is 0.1d0.

Blocker_scaling_factor = 0

de_Jager_scaling_factor

de Jager mass loss for various applications. de Jager, C., Nieuwenhuijzen, H., & van der Hucht, K. A. 1988, A&AS, 72, 259. Parameter for mass loss by de Jager wind prescription.

de_Jager_scaling_factor = 0d0

van_Loon_scaling_factor

see van Loon et al. 2005, A&A, 438, 273 “An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars”

van_Loon_scaling_factor = 0d0

Nieuwenhuijzen_scaling_factor

See Nieuwenhuijzen, H.; de Jager, C. 1990, A&A, 231, 134.

Nieuwenhuijzen_scaling_factor = 0d0

Vink_scaling_factor

Vink, J.S., de Koter, A., & Lamers, H.J.G.L.M., 2001, A&A, 369, 574. “Mass-loss predictions for O and B stars as a function of metallicity”

Vink_scaling_factor = 0d0

Bjorklund_scaling_factor

Björklund, R., Sundqvist, J.O., Puls, J., & Najarro, F., 2021, A&A, 648, A36. “New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars II. A grid of O-type stars in the Galaxy and the Magellanic Clouds”

This wind scheme does not feature a bistability jump.

Bjorklund_scaling_factor = 0d0

Dutch_scaling_factor

The “Dutch” wind scheme for massive stars combines results from several papers, all with authors mostly from the Netherlands.

The particular combination we use is based on Glebbeek, E., et al, A&A 497, 255-264 (2009) [more Dutch authors!]

For Teff > 1e4 and surface H > 0.4 by mass, use Vink et al 2001 Vink, J.S., de Koter, A., & Lamers, H.J.G.L.M., 2001, A&A, 369, 574.

For Teff > 1e4 and surface H < 0.4 by mass, use Nugis & Lamers 2000 Nugis, T.,& Lamers, H.J.G.L.M., 2000, A&A, 360, 227 Some folks use 0.8 for non-rotating models (Maeder & Meynet, 2001).

Dutch_scaling_factor = 0d0

Dutch_wind_lowT_scheme

For Teff < 1e4

Use de Jager if Dutch_wind_lowT_scheme = 'de Jager' de Jager, C., Nieuwenhuijzen, H., & van der Hucht, K. A. 1988, A&AS, 72, 259.

Use van Loon if Dutch_wind_lowT_scheme = 'van Loon' van Loon et al. 2005, A&A, 438, 273.

Use Nieuwenhuijzen if Dutch_wind_lowT_scheme = 'Nieuwenhuijzen' Nieuwenhuijzen, H.; de Jager, C. 1990, A&A, 231, 134

Dutch_wind_lowT_scheme = 'de Jager'

Kudritzki_scaling_factor

Radiation driven winds of hot stars. See Kudritzki et al, Astron. Astrophys. 219, 205-218 (1989). this is now implemented using the other_wind hook. see other_physics_hooks test case.

Grafener_scaling_factor

Grafener, G. & Hamann, W.-R. 2008, A&A 482, 945 contributed to mesa by Nilou Afsari this is now implemented using the other_wind hook. see other_physics_hooks test case.

Stern51_scaling_factor

this is now implemented using the other_wind hook. see other_physics_hooks test case.

use_accreted_material_j

Angular momentum of accreted material.

use_accreted_material_j = .false.

If false, then accreted material is given j so that it is rotating at the same angular velocity as the surface. If true, then accreted material is given j = accreted_material_j.

accreted_material_j = 0

no_wind_if_no_rotation

Use this to delay start of wind until after have started rotation.

no_wind_if_no_rotation = .false.

min_wind

Min wind in Msun/year > 0; ignore this limit if it is <= 0. e.g., might have low level wind even when normal scheme doesn’t call for any.

min_wind = 0d0

max_wind

Max wind in Msun/year > 0; ignore this limit if it is <= 0.

max_wind = 0d0

For critical rotation mass loss Redo step as needed to find mdot that brings model to just below critical. if max_mdot_redo_cnt > 0, and surf_omega_div_omega_crit > surf_omega_div_omega_crit_limit, then recompute the step while increasing mdot, until surf_omega_div_omega_crit < surf_omega_div_omega_crit_limit. Once an upper limit for mdot is found, the solution for mdot is further refined by bisection until it is computed to a tolerance of surf_omega_div_omega_crit_tol. During iterations, mdot is adjusted alternately by multiplication by mdot_revise_factor, and by adjusting it by implicit_mdot_boost*mdot_initial, where mdot_initial is the value of mdot at the first iteration. This is done to deal with mass accreting stars, where mdot might need to change sign for the star to remain below critical. This is a direct replacement for surf_w_div_w_crit_limit and surf_w_div_w_crit_tol

max_mdot_redo_cnt = 0
min_years_dt_for_redo_mdot = 0
surf_omega_div_omega_crit_limit = 0.99d0
surf_omega_div_omega_crit_tol = 0.05d0
mdot_revise_factor = 1.1d0
implicit_mdot_boost = 0.1d0

implicit wind computation.

max_tries_for_implicit_wind

The implicit method will modify the mass transfer rate and redo the step until it either finds a solution, or the number of tries hits max_tries_for_implicit_wind. If max_tries_for_implicit_wind = 0, the wind computation is explicit, meaning that the value of mdot is set using values at the start of the step. This only applies when mdot < 0.

max_tries_for_implicit_wind = 0

iwind_tolerance

Tolerance for which a solution is considered valid. A solution is valid if

abs(explicit_mdot - implicit_mdot) <
       abs(implicit_mdot)*iwind_tolerance

where

explicit_mdot = mstar_dot at start of step
implicit_mdot = mstar_dot at end of step

iwind_tolerance = 1d-3

iwind_lambda

If do not satisfy tolerance, redo with a different mdot as follows:

mstar_dot = explicit_mdot + &

iwind_lambda*(implicit_mdot - explicit_mdot)

iwind_lambda = 1d0

super_eddington_scaling_factor

For super eddington wind we use Ledd averaged by mass to optical depth tau = surf_avg_tau.

super_eddington_scaling_factor = 0

super_eddington_wind_Ledd_factor

Parameter for mass loss driven by super Eddington luminosity. Divide L by this factor when computing super Eddington wind, e.g., if this is 2, then only get wind when L/2 > Ledd.

super_eddington_wind_Ledd_factor = 1

wind_boost_full_off_L_div_Ledd

Boost off for L/Ledd <= this (set large to disable this). This alternative form is used when super_eddington_scaling_factor == 0.

wind_boost_full_off_L_div_Ledd = 1.5d0

wind_boost_full_on_L_div_Ledd

Do max boost for L/Ledd >= this. This alternative form is used when super_eddington_scaling_factor == 0.

wind_boost_full_on_L_div_Ledd = 5

super_eddington_wind_max_boost

Multiply wind mdot by up to this amount. This alternative form is used when super_eddington_scaling_factor == 0.

super_eddington_wind_max_boost = 1

trace_super_eddington_wind_boost

Send super eddington wind information to terminal.

trace_super_eddington_wind_boost = .false.

mass_change_full_on_dt

mass_change_full_off_dt

These params provide the option to turn off mass change when have very small timesteps. Between mass_change_full_on_dt and mass_change_full_off_dt mass change is gradually reduced. Units in seconds.

mass_change_full_on_dt = 1d-99
mass_change_full_off_dt = 1d-99

trace_dt_control_mass_change

trace_dt_control_mass_change = .false.

max_star_mass_for_gain

Automatic stops for mass loss/gain in Msun units (negative means ignore this parameter). Turn off mass gain when star mass reaches this limit.

max_star_mass_for_gain = -1

min_star_mass_for_loss

Automatic stops for mass loss/gain in Msun units (negative means ignore this parameter). Turn off mass loss when star mass reaches this limit.

min_star_mass_for_loss = -1

max_T_center_for_any_mass_loss

No mass loss for T center > this.

max_T_center_for_any_mass_loss = 2d9

max_T_center_for_full_mass_loss

No reduction in mass loss for T center <= this. This must be <= max_T_center_for_full_mass_loss. Reduce mass loss rate to 0 as T center climbs from max_for_full to max_for_any. The idea behind this is that during final stages of burning, there is so little time left in the life of the star, that any mass loss to winds will be negligible, but the inclusion of that insignificant mass loss can actually make convergence more difficult, so you are better off without it.

max_T_center_for_full_mass_loss = 1d9

wind_H_envelope_limit

Winds automatically shut off when star_mass - he_core_mass mass is less than this limit. The value of he_core_boundary_h1_fraction defines he_core_mass. Mass in Msun units. Previously called wind_envelope_limit.

wind_H_envelope_limit = -1

wind_H_He_envelope_limit

Winds automatically shut off when star_mass - co_core_mass is less than this limit. The value of co_core_boundary_he4_fraction defines co_core_mass. Mass in Msun units.

wind_H_He_envelope_limit = -1

wind_He_layer_limit

Winds automatically shut off when he_core_mass - co_core_mass is less than this limit. Mass in Msun units.

wind_He_layer_limit = -1

rlo_scaling_factor

Amplitude of mass loss. “rlo” wind scheme provides a simple radius-determined-wind with exponential increase.

rlo_scaling_factor = 0

rlo_wind_min_L

Only on when L > this limit. (Lsun)

rlo_wind_min_L = 1d-6

rlo_wind_max_Teff

Only on when Teff < this limit.

rlo_wind_max_Teff = 1d99

rlo_wind_roche_lobe_radius

Only on when R > this (Rsun).

rlo_wind_roche_lobe_radius = 0.40d0

rlo_wind_base_mdot

Base rate of mass loss when R = roche lobe radius (Msun/year).

rlo_wind_base_mdot = 1d-3

rlo_wind_scale_height

Determines exponential growth rate of mass loss (Rsun).

rlo_wind_scale_height = 1d-1

roche_lobe_xfer_full_on

Full accretion when R/RL <= this. Limit accretion when Roche lobe is nearing full (only with rlo_scaling_factor > 0).

roche_lobe_xfer_full_on = 0.5d0

roche_lobe_xfer_full_off

No accretion when R/RL >= this.

roche_lobe_xfer_full_off = 1.0d0

controls for adjust_mass

max_logT_for_k_below_const_q

max_q_for_k_below_const_q

min_q_for_k_below_const_q

Move k_below_const_q inward from surface until q(k) <= max_q. Then continue moving inward until reach logT(k) >= max_logT or q(k) <= min_q.

max_logT_for_k_below_const_q = 5
max_q_for_k_below_const_q = 1.0d0
min_q_for_k_below_const_q = 0.999d0

max_logT_for_k_const_mass

max_q_for_k_const_mass

min_q_for_k_const_mass

Move k_const_mass inward from k_below_const_q+1 until q(k) <= max_q. Then continue moving inward until reach logT(k) >= max_logT or q(k) <= min_q.

max_logT_for_k_const_mass = 6
max_q_for_k_const_mass = 1.0d0
min_q_for_k_const_mass = 0.995d0

composition controls

accrete_same_as_surface

If true, composition of accreted material is identical to the current surface composition. If false, then the composition is determined by accrete_given_mass_fractions.

The actual mass accretion rate can be set up using the mass_change option.

accrete_same_as_surface = .true.

accrete_given_mass_fractions

If true, use accrete_given_mass_fractions, num_accretion_species, accretion_species_id and accretion_species_xa to determine composition of accreted material – they must add to 1.0.

If false, then the composition is determined using accretion_h1, accretion_h2, accretion_he3, accretion_he4 and accretion_zfracs.

The actual mass accretion rate can be set up using the mass_change option.

Note that this control is ignored if accrete_same_as_surface is true.

accrete_given_mass_fractions = .false.

num_accretion_species

accretion_species_id

accretion_species_xa

If accrete_same_as_surface is false and accrete_given_mass_fractions is true, then composition of accreted material is determined by these options. The actual mass accretion rate can be set up using the mass_change option.

num_accretion_species can be up to s% max_num_accretion_species, see star/public/star_def.inc for the value of this parameter.

For each of num_accretion_species, the id for the isotope needs to be specified by accretion_species_id as defined in chem/public/chem_def.f90.

Mass fractions for each isotope are defined by accretion_species_xa

num_accretion_species = 0
accretion_species_id(1) = ''
accretion_species_xa(1) = 0

accretion_h1

accretion_h2

accretion_he3

accretion_he4

If accrete_same_as_surface is false and accrete_given_mass_fractions is false, then the mass fractions of h1, h2, he3 and h4 are determined by these options. Mass fractions for metals are set with the accretion_zfracs control. The actual mass accretion rate can be set up using the mass_change option.

If no h2 in current net, then it is automatically added to h1.

accretion_h1 = 0
accretion_h2 = 0
accretion_he3 = 0
accretion_he4 = 0

accretion_zfracs =

One of the following identifiers for different Z fractions from chem_def.

• AG89_zfracs = 1, Anders & Grevesse 1989

• GN93_zfracs = 2, Grevesse & Noels 1993

• GS98_zfracs = 3, Grevesse & Sauval 1998

• L03_zfracs = 4, Lodders 2003

• AGS05_zfracs = 5, Asplund, Grevesse & Sauval 2005

or set accretion_zfracs = 0 to use the following list of z fractions

accretion_zfracs = -1

accretion_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.

accretion_dump_missing_metals_into_heaviest = .true.

Special list of z fractions. If you use these, they must add to 1.0.

z_fraction_li = 0
z_fraction_be = 0
z_fraction_b = 0
z_fraction_c = 0
z_fraction_n = 0
z_fraction_o = 0
z_fraction_f = 0
z_fraction_ne = 0
z_fraction_na = 0
z_fraction_mg = 0
z_fraction_al = 0
z_fraction_si = 0
z_fraction_p = 0
z_fraction_s = 0
z_fraction_cl = 0
z_fraction_ar = 0
z_fraction_k = 0
z_fraction_ca = 0
z_fraction_sc = 0
z_fraction_ti = 0
z_fraction_v = 0
z_fraction_cr = 0
z_fraction_mn = 0
z_fraction_fe = 0
z_fraction_co = 0
z_fraction_ni = 0
z_fraction_cu = 0
z_fraction_zn = 0

lgT_lo_for_set_new_abundances

lgT_hi_for_set_new_abundances

Composition controls for set_new_abundances.

lgT_lo_for_set_new_abundances = 5.2d0
lgT_hi_for_set_new_abundances = 5.5d0

mesh adjustment

max_allowed_nz

Maximum number of grid points allowed. Array allowed to grow arbitrarily large if max_allowed_nz <= 0 If nz > max_allowed_nz, MESA will prematurely exit and call this error.

max_allowed_nz = 8000

remesh_max_allowed_logT

Turn off remesh if any cell has logT > this.

remesh_max_allowed_logT = 1d99

mesh_max_allowed_ratio

Must be >= 2.5. Max ratio for mass of adjacent cells. If have ratio exceeding this, split the larger cell.

mesh_max_allowed_ratio = 2.5d0

max_delta_x_for_merge

Don’t merge neighboring cells if any abundance differs by more than this.

max_delta_x_for_merge = 0.1d0

mesh_delta_coeff

A larger value increases the max allowed deltas and decreases the number of grid points. and a smaller does the opposite.

analogous to time_delta_coeff for better time resolution.

E.g., you’ll roughly double the number of grid points if you cut mesh_delta_coeff in half. Don’t expect it to exactly double the number however since other parameters in addition to gradients also influence the details of the grid spacing.

this factor also applies to max_dq, max_center_cell_dq, and max_surface_cell_dq.

mesh_delta_coeff = 1.0d0

mesh_Pgas_div_P_exponent

Multiply mesh_delta_coeff by (Pgas/Ptotal) to this power.

mesh_Pgas_div_P_exponent = 0

mesh_delta_coeff_for_highT

Use different mesh_delta_coeff at higher temperatures.

mesh_delta_coeff_for_highT = 3.0d0

logT_max_for_standard_mesh_delta_coeff

Use mesh_delta_coeff for center logT <= this. This value should be less than logT_min_for_highT_mesh_delta_coeff.

logT_max_for_standard_mesh_delta_coeff = 9.0d0

logT_min_for_highT_mesh_delta_coeff

Use mesh_delta_coeff_for_highT for center logT >= this. Linearly interpolate in logT for intermediate center temperatures.

logT_min_for_highT_mesh_delta_coeff = 9.5d0

max_dq

Max size for cell as fraction of total mass.

max_dq = 1d-2

min_dq

Min size for cell as fraction of total mass.

min_dq = 1d-14

Min size for cell to be split.

min_dq_for_split = 1d-14

min_dq_for_xa

Min size for splitting because of composition gradient. only for non-convective regions if have set min_dq_for_xa_convective > 0.

min_dq_for_xa = 1d-14

min_dq_for_xa_convective

Min size for splitting because of composition gradient in convective regions. if <= 0, then use min_dq_for_xa instead of this.

min_dq_for_xa_convective = 1d-6

Min size for cell to be split because of jump in logT.

min_dq_for_logT = 1d-14

mesh_min_dlnR

Limit on difference in lnR across cell for mesh refinement. Do not make this smaller than about 1d-14 or will fail with numerical problems.

mesh_min_dlnR = 1d-9

merge_if_dlnR_too_small

If true, mesh adjustment will force merge if difference in lnR across cell is too small.

merge_if_dlnR_too_small = .false.

mesh_min_dr_div_dRstar

Limit on relative radial extent for mesh refinement. dRstar = s% r(1) - s% R_center Don’t split if dr/dRstar would drop below this limit.

mesh_min_dr_div_dRstar = -1

merge_if_dr_div_dRstar_too_small

If true, mesh adjustment will force merge if dr_div_dRstar too small.

merge_if_dr_div_dRstar_too_small = .true.

mesh_min_dr_div_cs

Limit (in seconds) on sound crossing time for mesh refinement. Don’t split if sound crossing time would drop below this limit.

mesh_min_dr_div_cs = -1

merge_if_dr_div_cs_too_small

If true, mesh adjustment will force merge if dr_div_cs too small.

merge_if_dr_div_cs_too_small = .true.

max_center_cell_dq

Largest allowed dq at center.

max_center_cell_dq = 1d-7

max_surface_cell_dq

Largest allowed dq at surface.

max_surface_cell_dq = 1d-12

max_num_subcells

Limits number of new cells from 1 old one.

max_num_subcells = 2

max_num_merge_cells

Limits number of old cells to merge into 1 new one.

max_num_merge_cells = 2

mesh_adjust_get_T_from_E

If true, then use internal energy conservation to set new temperature. If false, just use average temperature based on reconstruction polynomials.

mesh_adjust_get_T_from_E = .true.

mesh_ok_to_merge

mesh_max_k_old_for_split

mesh_min_k_old_for_split

mesh_ok_to_merge = .true.
mesh_max_k_old_for_split = 999999999
mesh_min_k_old_for_split = 0

E_function_weight

internal energy gradient, E_function = E_function_weight*max(E_function_param,log10(energy)).

E_function_weight = 0
E_function_param = 16d0

P_function_weight

Pressure gradient, P_function = P_function_weight*log10(P).

P_function_weight = 40

T_function1_weight

Temperature gradient, T_function1 = T_function1_weight*log10(T). NOTE: The T gradient mesh controls below seems to be necessary to allow burning that starts off center to be able to reach the center. You can see this in the pre_zahb test_suite case if you try running it without the T function. The center temperature will fail to rise.

T_function1_weight = 110

T_function2_weight

T_function2_param

T_function2 = T_function2_weight*log10(T / (T + T_function2_param))

Largest change in T_function2 happens around T = T_function2_param. Default value puts this in the envelope ionization region.

T_function2_weight = 0
T_function2_param = 2d4

R_function_weight

R_function_param

log radius gradient

R_function = R_function_weight*log10(1 + (r/Rsun)/R_function_param)

R_function_weight = 0
R_function_param = 1d-4

R_function2_weight

R_function2_param1

R_function2_param2

R_function2 = R_function2_weight*min(R_function2_param1,max(R_function2_param2,r/Rstar))

where Rstar = radius of outer edge of model.

R_function2_weight = 0
R_function2_param1 = 0.4d0
R_function2_param2 = 0

R_function3_weight

radius gradient

R_function3 = R_function3_weight*(r/Rstar)

R_function3_weight = 0

M_function_weight

M_function_param

log mass gradient

M_function = M_function_weight*log10(1 + (m/Msun)/M_function_param)

M_function_weight = 0
M_function_param = 1d-6

gradT_function_weight

gradT gradient, gradT_function = gradT_function_weight*gradT

gradT_function_weight = 0

log_tau_function_weight

log_tau gradient (optical depth)

log_tau_function = log_tau_function_weight*log10(tau)

log_tau_function_weight = 0

log_kap_function_weight

log_kap gradient (optical depth)

log_kap_function = log_kap_function_weight*log10(kap)

log_kap_function_weight = 0

omega_function_weight

omega gradient (rotation omega in rad/sec)

omega_function = omega_function_weight*log10(omega)

omega_function_weight = 0

gam_function_weight

gam_function_param1

gam_function_param2

For extra resolution around liquid/solid transition.

gam = plasma interaction parameter
gam_function = gam_function_weight*tanh((gam - gam_function_param1)/gam_function_param2)

gam_function_weight = 0
gam_function_param1 = 170
gam_function_param2 = 20

xa_function_species

xa_function_weight

Mass fraction gradients.

xa_function = xa_function_weight*log10(xa + xa_function_param),

Up to num_xa_function of these - see star_def for value of num_xa_function. 0 length string means skip, otherwise name of nuclide as defined in chem_def. weight <= 0 means skip.

xa_function_species(:) = ''
xa_function_weight(:) = 0

xa_function_species(1) = 'he4'
xa_function_weight(1) = 30
xa_function_param(1) = 1d-2

xa_mesh_delta_coeff

Useful if you want to increase mesh_delta_coeff during advanced burning. If xa_function_species(j) has the largest atomic number in current set of species, then multiply mesh_delta_coeff by xa_mesh_delta_coeff(j).

xa_mesh_delta_coeff(:) = 1

mesh_delta_coeff_factor_smooth_iters

Some smoothing is useful when using local changes to mesh_delta_coeff.

mesh_delta_coeff_factor_smooth_iters = 3

“Indirect” mesh controls work by increasing sensitivity in selected regions. They work in the same way as mesh_delta_coeff – values less than 1.0 mean smaller allowed jumps in mesh functions and hence smaller grid points and higher resolution. But whereas mesh_delta_coeff applies uniformly to all cells, the “extra” coefficients can vary in value from one cell to the next.

Note that you can set your own local changes by means of the hook other_mesh_delta_coeff_factor.

mesh_logX_species

mesh_logX_min_for_extra

Increase resolution at points with large abs(dlogX/dlogP); logX = log10(X mass fraction).

mesh_logX_species(1) = ''
mesh_logX_min_for_extra(1) = -6

mesh_dlogX_dlogP_extra(1)

mesh_dlogX_dlogP_full_on(1)

mesh_dlogX_dlogP_full_off(1)

Only increase resolution if logX >= mesh_logX_min_for_extra. Make mesh_dlogX_dlogP_extra < 1 for smaller allowed change in logP and hence higher resolution. Full effect if abs(dlogX/dlogP) >= mesh_dlogX_dlogP_full_on. No effect if abs(dlogX/dlogP)) <= mesh_dlogX_dlogP_full_off. Up to num_mesh_logX of these (see star_def for value of num_mesh_logX).

mesh_dlogX_dlogP_extra(1) = 1
mesh_dlogX_dlogP_full_on(1) = 2
mesh_dlogX_dlogP_full_off(1) = 1

Multiply mesh_delta_coeff near convection zone boundary (czb) by the following factors. Value < 1 gives increased resolution.

Increase resolution at points with large abs(dlog_eps/dlogP) for nuclear power eps (ergs/g/sec). At any particular location, only use eps nuc category with max local value e.g., only use mesh_dlog_pp_dlogP_extra at points where pp is the max burn source.

mesh_dlog_eps_min_for_extra

Only increase resolution if log_eps >= mesh_dlog_eps_min_for_extra.

mesh_dlog_eps_min_for_extra = -2

mesh_dlog_eps_dlogP_full_on

Full effect if abs(dlog_eps/dlogP) >= mesh_dlog_eps_dlogP_full_on.

mesh_dlog_eps_dlogP_full_on = 4

mesh_dlog_eps_dlogP_full_off

No effect if abs(dlog_eps/dlogP)) <= mesh_dlog_eps_dlogP_full_off.

mesh_dlog_eps_dlogP_full_off = 1

Multiply the allowed change between adjacent cells by the following factors; (small factor => smaller allowed change => more cells).

pp and cno burning

mesh_dlog_pp_dlogP_extra = 0.25d0
mesh_dlog_cno_dlogP_extra = 0.25d0

triple alpha, c, n, and o burning

mesh_dlog_3alf_dlogP_extra = 0.25d0
mesh_dlog_burn_c_dlogP_extra = 0.25d0
mesh_dlog_burn_n_dlogP_extra = 0.25d0
mesh_dlog_burn_o_dlogP_extra = 0.25d0

ne, na, and mg burning

mesh_dlog_burn_ne_dlogP_extra = 0.25d0
mesh_dlog_burn_na_dlogP_extra = 0.25d0
mesh_dlog_burn_mg_dlogP_extra = 0.25d0

c12+c12. c12+o16, and o16+o16 burning

mesh_dlog_cc_dlogP_extra = 0.25d0
mesh_dlog_co_dlogP_extra = 0.25d0
mesh_dlog_oo_dlogP_extra = 0.25d0

si to iron along alpha chain burning

mesh_dlog_burn_si_dlogP_extra = 0.25d0
mesh_dlog_burn_s_dlogP_extra = 0.25d0
mesh_dlog_burn_ar_dlogP_extra = 0.25d0
mesh_dlog_burn_ca_dlogP_extra = 0.25d0
mesh_dlog_burn_ti_dlogP_extra = 0.25d0
mesh_dlog_burn_cr_dlogP_extra = 0.25d0
mesh_dlog_burn_fe_dlogP_extra = 0.25d0

photodisintegration burning

mesh_dlog_pnhe4_dlogP_extra = 0.25d0
mesh_dlog_other_dlogP_extra = 0.25d0
mesh_dlog_photo_dlogP_extra = 1

convective_bdy_weight

convective_bdy_dq_limit

convective_bdy_min_dt_yrs

Mesh function to enhance resolution near convective boundaries

convective_bdy_weight = 0
convective_bdy_dq_limit = 3d-5
convective_bdy_min_dt_yrs = 1d-3

max_rel_delta_IE_for_mesh_total_energy_balance

remeshing can adjust internal energy of cell by this fraction in order to maintain total internal + potential + kinetic energy.

max_rel_delta_IE_for_mesh_total_energy_balance = 0.05d0

trace_mesh_adjust_error_in_conservation

If true, report relative errors for total PE, KE, and IE. (potential, kinetic, internal).

trace_mesh_adjust_error_in_conservation = .false.

okay_to_remesh

If false, then no remeshing.

okay_to_remesh = .true.

restore_mesh_on_retry

If true, then after a retry the remeshing is undone for the step, and the following try is performed with the same mesh used in the previous step. This can help with the retry by reducing the changes.

restore_mesh_on_retry = .false.

num_steps_to_hold_mesh_after_retry

When restore_mesh_on_retry=true, then after a retry remeshing is not done for this number of steps.

num_steps_to_hold_mesh_after_retry = 0

remesh_dt_limit

No remesh if dt < remesh_dt_limit, in seconds.

remesh_dt_limit = -1

use_split_merge_amr

use_split_merge_amr = .false.

split_merge_amr_logtau_zoning

split_merge_amr_log_zoning

split_merge_amr_hybrid_zoning

split_merge_amr_flipped_hybrid_zoning

if split_merge_amr_logtau_zoning, target is even grid spacing in logtau else if split_merge_amr_log_zoning, target is even grid spacing in logr else if split_merge_amr_hybrid_zoning, target is even r spacing for core, even logr outside else if split_merge_amr_flipped_hybrid_zoning, target is even logr spacing for core, even r outside else target is even grid spacing in r

split_merge_amr_logtau_zoning = .false.
split_merge_amr_log_zoning = .true.
split_merge_amr_hybrid_zoning = .false.
split_merge_amr_flipped_hybrid_zoning = .false.

split_merge_amr_nz_baseline

split_merge_amr_nz_r_core

split_merge_amr_nz_r_core_fraction

split_merge_amr_mesh_delta_coeff

split_merge_amr_nz_baseline = 1000
split_merge_amr_nz_r_core = 0d0 ! ignore if <= 0
split_merge_amr_nz_r_core_fraction = 0d0 ! ignore if <= 0; else r_core = r_center + fraction*(r(1) - r_center)
split_merge_amr_mesh_delta_coeff = 1d0 ! like mesh_delta_coeff, but for amr

split_merge_amr_MaxLong

split_merge_amr_MaxShort

split cell if ratio of actual/desired size is > split_merge_amr_MaxLong; ignore if <= 0 merge cell if ratio of desired/actual size is < split_merge_amr_MaxShort; ignore if <= 0 be careful to avoid inconsistent limits such as when a required split triggers a required merge. to be safe, make sure product of limits > 2.

split_merge_amr_MaxLong = 1.5d0
split_merge_amr_MaxShort = 1.5d0

merge_amr_max_abs_du_div_cs

merge_amr_max_abs_du_div_cs = 0.1d0

merge_amr_du_div_cs_limit_only_for_compression

If true, then merge_amr_max_abs_du_div_cs limit will only be considered for cells that would undergo compression

merge_amr_du_div_cs_limit_only_for_compression = .false.

merge_amr_inhibit_at_jumps

merge_amr_inhibit_at_jumps = .false.

merge_amr_ignore_surface_cells

merge_amr_k_for_ignore_surface_cells

Merging surface cells can cause problems. If merge_amr_ignore_surface_cells is true, then the outermost merge_amr_k_for_ignore_surface_cells cells are ignored for merge.

merge_amr_ignore_surface_cells = .true.
merge_amr_k_for_ignore_surface_cells = 2

split_merge_amr_avoid_repeated_remesh

If true, then after a cell has been merged or split, the resulting cell will not be considered in further remeshing for this step.

split_merge_amr_avoid_repeated_remesh = .false.

split_merge_amr_dq_min

split_merge_amr_dq_max

split_merge_amr_dq_min = 1d-14
split_merge_amr_dq_max = 1d0

split_merge_amr_r_core_cm

split_merge_amr_r_core_cm = 1d8

split_merge_amr_max_iters

split_merge_amr_max_iters = 100

split_merge_amr_okay_to_split_1

split_merge_amr_okay_to_split_nz

split_merge_amr_okay_to_split_1 = .true.
split_merge_amr_okay_to_split_nz = .true.

equal_split_density_amr

equal_split_density_amr = .false.

trace_split_merge_amr

trace_split_merge_amr = .false.

nuclear reaction controls

default_net_name

Name of base reaction network. Each net corresponds to a file in $MESA_DIR/data/net_data/nets. Look in that directory to see your network options, or learn how to create your own net.

default_net_name = 'basic.net'

screening_mode

• empty string means no screening

• ' extended' : extends the Graboske (1973) method using results from Alastuey and Jancovici (1978), along with plasma parameters from Itoh et al (1979) for strong screening.

• 'salpeter' : weak screening only. following Salpeter (1954), with equations (4-215) and (4-221) of Clayton (1968).

• 'chugunov' : based on code from Sam Jones Implements screening from Chugunov et al (2007) for weak and strong screening MESA versions <=11435 used extended as the default value

screening_mode = 'chugunov'

net_logTcut_lo

strong rates are zero logT < logTcut_lo use default from net if this is <= 0

net_logTcut_lo = -1

net_logTcut_lim

strong rates cutoff smoothly for logT < logTcut_lim use default from net if this is <= 0

net_logTcut_lim = -1

max_abar_for_burning

if abar > this, suppress all burning e.g., if want an “inert” core heavy elements, set this to 55 or, if want to turn off the net, set this to -1

max_abar_for_burning = 199

dxdt_nuc_factor

Control for abundance changes by burning. Changes dxdt_nuc (rate of change of abundances) without changing the rates or eps_nuc (rate of energy generation).

dxdt_nuc_factor = 1

weak_rate_factor

all weak rates are multiplied by this factor

weak_rate_factor = 1

reaction_neuQs_factor

all neutrino Q factors are multiplied by this factor

reaction_neuQs_factor = 1

nonlocal_NiCo_kap_gamma

nonlocal_NiCo_kap_gamma = 0

nonlocal_NiCo_decay_heat

if true, do non-local deposition of gamma-ray energy from Ni56 and Co56 decays. only for approx nets including co56. intended for use with stripped envelope supernovae.

nonlocal_NiCo_decay_heat = .false.

dtau_gamma_NiCo_decay_heat

dtau_gamma_NiCo_decay_heat = 1d0

max_logT_for_net

max_logT_for_net = 10.2d0

element diffusion

gravitational settling and chemical diffusion.

show_diffusion_info

terminal output for diffusion

show_diffusion_info = .false.

show_diffusion_substep_info

terminal output for diffusion

show_diffusion_substep_info = .false.

show_diffusion_timing

show time for each call on diffusion

show_diffusion_timing = .false.

do_element_diffusion

determines whether or not we do element diffusion

do_element_diffusion = .false.

diffusion_dt_limit

no element diffusion if dt < this limit (in seconds)

diffusion_dt_limit = 3.15d7

diffusion_use_paquette

if true, use atomic diffusion coefficients according to Paquette et al. (1986). if false, use Stanton & Murillo PhRvE, 93, 043203 (2016) for diffusion coefficients. (Paquette coefficients still used for electron-ion because Stanton & Murillo did not do calculations for attractive potentials.)

diffusion_use_paquette = .false.

diffusion_use_caplan

if true, use atomic diffusion coefficients according to Caplan, Bauer, & Freeman MNRAS, 513, L52 (2022) at strong coupling (Gamma > 10), relevant for white dwarf interiors.

diffusion_use_caplan = .true.

diffusion_use_iben_macdonald

if true, use diffusion coefficients similar to Iben & MacDonald (1985). if false, use Stanton & Murillo (2016) for diffusion coefficients. this was previously called diffusion_use_pure_coulomb.

diffusion_use_iben_macdonald = .false.

diffusion_use_cgs_solver

if false, solve the system of equations described by Thoul et al. (1994) if true, solve the unmodified Burgers equations in cgs units

diffusion_use_cgs_solver = .true.

cgs_thermal_diffusion_eta_full_on

cgs_thermal_diffusion_eta_full_off

When diffusion_use_cgs_solver = .true. for eta < cgs_thermal_diffusion_eta_full_on, includes the heat flow vector terms in the Burgers equations. Then smoothly turns off use of these terms so that they are not included for eta > cgs_thermal_diffusion_eta_full_off, since these terms are problematic when distribution function become non-Maxwellian.

cgs_thermal_diffusion_eta_full_on = 0d0
cgs_thermal_diffusion_eta_full_off = 2d0

do_WD_sedimentation_heating

min_xa_for_WD_sedimentation_heating

if true, include heating associated with sedimentation when element diffusion is on. Only elements with mass fraction > min_xa_for_WD_sedimentation_heating will be included in this calculation. For best results, set diffusion_use_full_net = .true. This will affect white dwarf cooling times. See also eps_WD_sedimentation_factor

do_WD_sedimentation_heating = .false.
min_xa_for_WD_sedimentation_heating = 1d-5

do_diffusion_heating

if true, calculate heating term associated with changes in internal energy due to any abundance changes from element diffusion, and include this term in the energy equation. To avoid double-counting, this control can only be used if do_WD_sedimentation_heating = .false.

do_diffusion_heating = .true.

diffusion_min_dq_at_surface

treat at least this much at surface as a single cell for purposes of diffusion

diffusion_min_dq_at_surface = 1d-9

diffusion_min_T_at_surface

treat cells cells at surface with T < this as a single cell for purposes of diffusion default should be large enough to ensure hydrogen ionization

diffusion_min_T_at_surface = 1d4

diffusion_min_dq_ratio_at_surface

combine cells at surface until have total mass >= this factor times the next cell below them this helps with surface boundary condition for diffusion by putting large cell at surface

diffusion_min_dq_ratio_at_surface = 10

diffusion_dt_div_timescale

dt is at most this fraction of timescale. Each stellar evolution step can be divided into many substeps for diffusion. The substep timescale is set by rates of flow in and out for each species in each cell. The substep size, dt, is initially set to timescale*diffusion_dt_div_timescale.

diffusion_dt_div_timescale = 1

diffusion_min_num_substeps

Max substep dt is total time divided by this.

diffusion_min_num_substeps = 1

diffusion_max_iters_per_substep

If the substep requires too many iterations, the substep time is decreased for a retry.

diffusion_max_iters_per_substep = 10

diffusion_max_retries_per_substep

If the substep requires too many retries, diffusion fails and forces a retry for the star.

diffusion_max_retries_per_substep = 10

diffusion_tol_correction_max

diffusion_tol_correction_norm

Tolerances for solver iterations. Corrections smaller will be treated as converged. Corrections larger will cause another solver iteration.

diffusion_tol_correction_max = 1d-1
diffusion_tol_correction_norm = 1d-3

diffusion_min_X_hard_limit

tolerance for negative mass fraction errors errors larger will cause retry; errors smaller will be corrected. Tightening this control may help with “failed in fixup” errors when diffusion_use_isolve = .true.

diffusion_min_X_hard_limit = -1d-3

diffusion_X_total_atol

diffusion_X_total_rtol

tolerances for errors in total species conservation errors larger will cause retry; errors smaller will be corrected.

diffusion_X_total_atol = 1d-9
diffusion_X_total_rtol = 1d-6

diffusion_upwind_abs_v_limit

switch to upwind for i at face k if abs(v(i,k)) > this limit mainly for use with radiative levitation where get very much higher velocities

diffusion_upwind_abs_v_limit = 1d99

diffusion_v_max

Max velocity (cm/sec). We can get extremely large velocities in the extreme outer envelope that cause problems numerically without really effecting the results, so we allow a max for the velocities that should help the numerics without changing the results. Note: change diffusion_v_max to at least 1d-2 when using radiative levitation.

diffusion_v_max = 1d-3

D_mix_ignore_diffusion

Diffusion is turned off in core and surface convection zones, since it is overwhelmed by other mixing there. D_mix_ignore_diffusion roughly defines the mixing coefficient below which diffusion is included again. The code finds the location where D_mix falls to this value, backs up some, and turns on diffusion from there onward.

D_mix_ignore_diffusion = 1d5

diffusion_gamma_full_off

diffusion_gamma_full_on

gamma_full_on <= gamma_full_off Shut off diffusion for large gamma (i.e. for gamma >= gamma_full_off). Gradually decrease diffusion as gamma increases from full_on to full_off. Allow normal diffusion for gamma <= gamma_full_on. Default is diffusion off when get well into liquid regime.

diffusion_gamma_full_off = 1d99
diffusion_gamma_full_on = 1d99

diffusion_T_full_on

diffusion_T_full_off

T_full_on >= T_full_off Shut off diffusion for small T (i.e., for T <= T_full_off) Gradually decrease diffusion as T decreases from T_full_on to T_full_off. Allow normal diffusion for T >= T_full_on.

diffusion_T_full_on = 1d3
diffusion_T_full_off = 1d3

diffusion_calculates_ionization

If diffusion_calculates_ionization is false, MESA uses typical charges for a set of representative species as defined in diffusion_class_typical_charge and diffusion_class_representative for all points rather than calculating the ionization from the local conditions.

diffusion_calculates_ionization = .true.

diffusion_nsmooth_typical_charge

smoothing over charge

diffusion_nsmooth_typical_charge = 10

diffusion_SIG_factor

diffusion_GT_factor

factors for playing with SIG and GT terms for concentration diffusion and advection

diffusion_SIG_factor = 1d0
diffusion_GT_factor = 1d0

diffusion_AD_dm_full_on

diffusion_AD_dm_full_off

diffusion_AD_boost_factor

artificial concentration diffusion near surface (mainly for radiative levitation) Msun units for full_on and full_off boost only used if > 0

diffusion_AD_dm_full_on = -1
diffusion_AD_dm_full_off = -1
diffusion_AD_boost_factor = 0

diffusion_Vlimit_dm_full_on

diffusion_Vlimit_dm_full_off

in Msun units artificial velocity limitation near surface (mainly for radiative levitation)

diffusion_Vlimit_dm_full_on = -1
diffusion_Vlimit_dm_full_off = -1

diffusion_Vlimit

In units of local cell crossing velocity (only used if > 0). When full on, limit abs(v) <= Vlimit*dr/dt, cell size dr, substep time dt.

diffusion_Vlimit = 0

D_mix_zero_region_bottom_q

D_mix_zero_region_top_q

dq_D_mix_zero_at_H_He_crossover

dq_D_mix_zero_at_H_C_crossover

D_mix_zero_region_bottom_q = 1d99
D_mix_zero_region_top_q = -1d99
dq_D_mix_zero_at_H_He_crossover = -1d0
dq_D_mix_zero_at_H_C_crossover = -1d0

diffusion_min_T_for_radaccel

diffusion_max_T_for_radaccel

If T between these limits, then include radiative levitation at that location. Calculation of radiative levitation is costly, so only use it where necessary. Note: change diffusion_v_max to at least 1d-2 when using radiative levitation.

Note that radiative levitation requires OP calculations of g_rad for each class, and only 17 elements are supported (H, He, C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Cr, Mn, Fe, Ni). If you want to include radiative levitation, your options are: + Define diffusion classes such that all class representatives are among the 17 elements listed above. + Use a net with only elements from the 17 above, and set diffusion_use_full_net = .true.

diffusion_min_T_for_radaccel = 0
diffusion_max_T_for_radaccel = 0

diffusion_min_Z_for_radaccel

diffusion_max_Z_for_radaccel

If Z between these limits, then include radiative levitation for that element. Calculation of radiative levitation is costly, so only use it where necessary. e.g., limit to Fe and Ni by min_Z = 26 and max_Z = 28

diffusion_min_Z_for_radaccel = 0
diffusion_max_Z_for_radaccel = 1000

diffusion_screening_for_radaccel

Include screening for radiative levitation.

diffusion_screening_for_radaccel = .true.

diffusion_use_full_net

If true, don’t lump elements into classes for diffusion. Instead, each isotope in the network is treated as its own separate class. This can cause significant slowdowns for large nets, so it is off by default. This works for nets with up to 100 isotopes; larger nets require lumping into classes.

diffusion_use_full_net = .false.

diffusion_num_classes

Number of representative classes of species for diffusion calculations. (maximum of 100)

diffusion_num_classes = 5

diffusion_class_representative(:)

isotope names for diffusion representatives

diffusion_class_representative(1) = 'h1'
diffusion_class_representative(2) = 'he3'
diffusion_class_representative(3) = 'he4'
diffusion_class_representative(4) = 'o16'
diffusion_class_representative(5) = 'fe56'

diffusion_class_A_max(:)

atomic number A. in ascending order. species goes into 1st class with A_max >= species A

diffusion_class_A_max(1) = 2
diffusion_class_A_max(2) = 3
diffusion_class_A_max(3) = 4
diffusion_class_A_max(4) = 16
diffusion_class_A_max(5) = 10000

diffusion_class_typical_charge(:)

Typical charges for use if diffusion_calculates_ionization is false Use charge 21 for Fe in the sun, from Thoul, Bahcall, and Loeb (1994), ApJ, 421, 828.

diffusion_class_typical_charge(1) = 1
diffusion_class_typical_charge(2) = 2
diffusion_class_typical_charge(3) = 2
diffusion_class_typical_charge(4) = 8
diffusion_class_typical_charge(5) = 21

diffusion_class_factor(:)

Arbitrarily enhance or inhibit diffusion effects by class.

diffusion_class_factor(:) = 1d0

parameters for ionization solver

diffusion_use_isolve

Activate iterative solver.

diffusion_use_isolve = .false.

diffusion_rtol_for_isolve

diffusion_atol_for_isolve

Relative and absolute error parameters for iterative solver.

diffusion_rtol_for_isolve = 1d-4
diffusion_atol_for_isolve = 1d-5

diffusion_maxsteps_for_isolve

Maximum number of steps to take in iterative solver.

diffusion_maxsteps_for_isolve = 1000

diffusion_isolve_solver

Which ode solver to use for iterative.

Options include:

• 'ros2_solver'

• 'rose2_solver'

• 'ros3p_solver'

• 'ros3pl_solver'

• 'rodas3_solver'

• 'rodas4_solver'

• 'rodasp_solver'

diffusion_isolve_solver = 'ros2_solver'

diffusion_dump_call_number

debugging info of diffusion at call number

diffusion_dump_call_number = -1

WD phase separation

do_phase_separation

Phase separation upon crystallization in WD cores using the implementation of Bauer (2023).

do_phase_separation = .false.

phase_separation_option

Choice of appropriate option for the WD core mixture:

• 'CO' : carbon-oxygen phase separation using the two-component phase diagram of Blouin & Daligault (2021a).

• 'ONe' : oxygen-neon phase separation using the two-component phase diagram of Blouin & Daligault (2021b).

phase_separation_option = 'CO'

do_phase_separation_heating

if true, calculate heating term associated with changes in internal energy due to any abundance changes from phase separation, and include this term in the energy equation.

do_phase_separation_heating = .true.

phase_separation_mixing_use_brunt

if true, the phase separation mixing recalculates relevant EOS quantities and evaluates the Ledoux criterion, including the brunt B term that depends on the composition gradient. This can be somewhat expensive, so this option can be set to false to instead just mix outward until there is no more negative mu gradient. These will produce similar final chemical profiles, but setting this option to true is the only way to properly evaluate the physical criterion.

phase_separation_mixing_use_brunt = .true.

eos controls

fix_d_eos_dxa_partials

The star solver uses the partial derivatives of lnPgas and lnE with respect to composition. When the EOS fails to provide these, replace them with a finite-difference approximation.

fix_d_eos_dxa_partials = .true.

opacity controls

more opacity controls can be found in star_job.defaults

use_simple_es_for_kap

for experiments with simple electron scattering if true, opacity = 0.2*(1 + X)

use_simple_es_for_kap = .false.

use_starting_composition_for_kap

for experiments with partials of opacity with respect to composition if true, calls on kap during solver iterations use the starting composition

use_starting_composition_for_kap = .false.

opacity_min

limit minimum opacities to this value (ignore this if value is < 0)

opacity_min = -1

opacity_max

limit opacities to this value (ignore this if value is < 0)

opacity_max = -1

opacity_factor

opacities are multiplied by this value

opacity_factor = 1

min_logT_for_opacity_factor_off

min_logT_for_opacity_factor_on and

max_logT_for_opacity_factor_on

max_logT_for_opacity_factor_off

temperature controls for where the opacity_factor is applied if, for example, you only want the opacity factor to apply in the iron bump region you can give a logT range such as

min_logT_for_opacity_factor_off = 5.2
min_logT_for_opacity_factor_on = 5.3
max_logT_for_opacity_factor_on = 5.7
max_logT_for_opacity_factor_off = 5.8

ignore these if < 0.

min_logT_for_opacity_factor_off = -1
min_logT_for_opacity_factor_on = -1
max_logT_for_opacity_factor_on = -1
max_logT_for_opacity_factor_off = -1

if you need cell-by-cell control of opacity factor, set the vector “extra_opacity_factor” using the routine “other_opacity_factor”

OP mono opacities

The OP_mono opacities use data and code from the OP website as modified by Haili Hu. Since the tar.xz file is large (462 MB), it is not included in the standard mesa download.

You can get OP4STARS_1.3.tar.xz from https://zenodo.org/records/4390522

Put it any place you want on your disk.

tar -xf OP4STARS_1.3.tar.xz

Set the inlist controls for the “mono” directory with the data files. For example, in my case it looks like the following, but you can put the directory anywhere you like – it doesn’t need to be in the mesa/data directory. And the cache file doesn’t need to be in the mono directory.

op_mono_data_path = '/Users/bpaxton/OP4STARS_1.3/mono'
op_mono_data_cache_filename = '/Users/bpaxton/OP4STARS_1.3/mono/op_mono_cache.bin'

If you use these opacities, you should cite Seaton (2005).

op_mono_data_path

if this path is set to the empty string, ‘’, then it defaults to the environment variable $(MESA_OP_MONO_DATA_PATH)

op_mono_data_path = ''      ! '' defaults to $MESA_OP_MONO_DATA_PATH

op_mono_data_cache_filename

if this is set to the empty string, ‘’, then it defaults to the environment variable $(MESA_OP_MONO_DATA_CACHE_FILENAME)

op_mono_data_cache_filename = ''      ! '' defaults to $MESA_OP_MONO_DATA_CACHE_FILENAME

op_mono_method

Compute the Rosseland mean opacity and radiative accelerations from the OP mono data by brute force ('hu') or use the faster method by allowing for a small tolerance on the mixture used for the computations of these variables ('mombarg').

op_mono_method = 'hu'

emesh_data_for_op_mono_path

path to the OP_mono_master_grid_MESA_emesh.txt file containing the data need for when op_mono_method = 'mombarg'. If this is set to the empty string, ‘’, then it defaults to the environment variable $(MESA_OP_MONO_MASTER_GRID)

You can get OP_mono_master_grid_MESA_emesh.txt from https://doi.org/10.5281/zenodo.6850861

You can either download the uncompressed .txt file, or download the compressed .xz file and then unpack it in place with unxz -v OP_mono_master_grid_MESA_emesh.txt.xz

emesh_data_for_op_mono_path = ''      ! '' defaults to $MESA_OP_MONO_MASTER_GRID

high_logT_op_mono_full_off

high_logT_op_mono_full_on

low_logT_op_mono_full_off

low_logT_op_mono_full_on

Blending controls for turning op_mono opacities off above (high_logT) and below (low_logT) specified temperature ranges. When not using op_mono, the code will use standard opacity tables. For example, you might only use high T limits so that op_mono is only used in the envelope, or you might set both low and high T limits so that op_mono is used around the Fe peak logT but not for other locations in the star. These controls should satisfy the following inequalities:

high_logT_op_mono_full_off >= high_logT_op_mono_full_on
high_logT_op_mono_full_on >= low_logT_op_mono_full_on
low_logT_op_mono_full_on >= low_logT_op_mono_full_off

op_mono opacities fully on if

log10T <= high_logT_op_mono_full_on and log10T >= low_logT_op_mono_full_on

op_mono opacities full off if

log10T >= high_logT_op_mono_full_off or log10T <= low_logT_op_mono_full_off

Note: OP mono ignored if either high_logT control < 0

high_logT_op_mono_full_off = -99
high_logT_op_mono_full_on = -99

low_logT_op_mono_full_off = -99
low_logT_op_mono_full_on = -99

op_mono_min_X_to_include

skip iso if mass fraction < this

op_mono_min_X_to_include = 1d-20

use_op_mono_alt_get_kap

if true, call the op_mono_alt_get_kap routine instead of op_mono_get_kap. see mesa/kap/public/kap_lib.f for details about these routines.

use_op_mono_alt_get_kap = .false.

min_kap_for_dPrad_dm_eqn

min_kap_for_dPrad_dm_eqn = 1d-4

asteroseismology controls

get_delta_nu_from_scaled_solar

If get_delta_nu_from_scaled_solar is .false., the large separation delta_nu is the inverse of the sound crossing time from one side of the star to the other, through the center. This is sometimes called the “asymptotic” large separation.

Otherwise, delta_nu is calculated from the asteroseismic scaling relations (see Ulrich 1986, Brown et al. 1991 and Kjeldsen & Bedding 1995) using solar reference values nu_max_sun, delta_nu_sun and astero_Teff_sun.

nu_max is always computed from the scaling relation.

get_delta_nu_from_scaled_solar = .false.

nu_max_sun

delta_nu_sun

astero_Teff_sun

Solar reference values used in the asteroseismic scaling relations for delta_nu (if get_delta_nu_from_scaled_solar is .false.) and nu_max (always).

The default nu_max_sun is the Sun-as-as-star value reported by Lund et al. (2017), which is consistent with but conceptually different from the result of 3073.59 ± 0.18 μHz by Kiefer et al. (2018).

The default delta_nu_sun is also taken from Lund et al. (2017).

The default astero_Teff_sun is the value adopted in IAU 2015 Resolution B3. This should not be confused with the constant Teffsun, which is always equal to the IAU value and not controlled by a parameter. The “asteroseismic” value can be changed in case one needs to reproduce previous calculations using the scaling relations.

nu_max_sun = 3078d0 ! μHz
delta_nu_sun = 134.91d0 ! μHz
astero_Teff_sun = 5772d0 ! kelvin

delta_Pg_traditional

delta_Pg_mode_freq

For calculating the asymptotic g-mode period spacing delta_Pg

if delta_Pg_traditional = .true., then calculate the asymptotic gravity mode period space by directly integrating N2 over the entire stellar model.

if delta_Pg_traditional = .false. use the method of Bildsten et al. (2012): //ui.adsabs.harvard.edu/abs/2012ApJ…744L…6B/abstract

delta_Pg_mode_freq is only used when delta_Pg_traditional = .false. it is provided in units of uHz. if <=0, use nu_max from scaled solar value

delta_Pg_traditional = .true.
delta_Pg_mode_freq = 0d0

Brunt controls

calculate_Brunt_B

calculate_Brunt_N2

Only calculate if this is true.

calculate_Brunt_B = .true.
calculate_Brunt_N2 = .true.

brunt_N2_coefficient

Standard N2 is multiplied by this value.

brunt_N2_coefficient = 1

num_cells_for_smooth_brunt_B

Number of cells on either side to use in weighted smoothing of brunt_B.

num_cells_for_smooth_brunt_B = 2

threshold_for_smooth_brunt_B

Threshold for weighted smoothing of brunt_B. Only apply smoothing (controlled by num_cells_for_smooth_brunt_B) for contiguous regions where \(|B|\) exceeds this threshold. Might be useful for preventing narrow peaks from being excessively broadened by smoothing

threshold_for_smooth_brunt_B = 0d0

min_magnitude_brunt_B

If set brunt_B to 0 if absolute value is < this.

min_magnitude_brunt_B = -1d99

structure equations

energy_eqn_option

Available options are 'dedt' or 'eps_grav'. See below for descriptions of each form and form-specific options.

energy_eqn_option = 'dedt'

dedt form

This form of the energy equation is used when energy_eqn_option = 'dedt'.

It is a conservative equation for the local specific total energy introduced in MESA V, Section 3. See in particular Eq. (8) and surrounding discussion.

Because this equation is written in a conservative form, it should always do an excellent job of numerical energy conservation. The error in numerical energy conservation (quantified by rel_E_err) reflects the energy equation residuals (i.e., the extent to which the energy equation was not satisfied). When using this form of the equation, models should generally have a small (\(\lesssim 10^{-8}\)) value of rel_E_err, roughly independent of space and time resolution. A small value of rel_E_err and its cumulative counterpart rel_run_E_err only demonstrates that the equation residuals are small and is not evidence that a model is converged or reliable. Convergence studies targeting the physical quantities of interest remain essential. A large value of rel_run_E_err (\(\gtrsim 10^{-2}\)) should be a cause for concern and should be investigated further (see also warn_when_large_rel_run_E_err and max_abs_rel_run_E_err )

no_dedt_form_during_relax

dedt_eqn_r_scale

no_dedt_form_during_relax = .true.
dedt_eqn_r_scale = 1d8

eps_grav form

This form of the energy equation is used when energy_eqn_option = 'eps_grav'.

The quantity eps_grav is defined as \(\epsilon_{\rm grav} = -\frac{De}{Dt} - P \frac{DV_\rho}{Dt}\), where \(e\) is the specific internal energy, \(P\) is the pressure, \(V_\rho \equiv 1/\rho\) is the specific volume, and \(D/Dt\) is the Lagrangian time derivative. See MESA IV, Section 8 for more discussion.

This quantity is then re-written into the following convenient-to-evaluate form (see MESA IV, eq. 63):

\(\epsilon_{\rm grav} = -T c_P \left[(1 - \nabla_{\rm ad} \chi_T)\frac{D\ln T}{Dt} - \nabla_{\rm ad} \chi_\rho \frac{D\ln \rho}{Dt}\right] + \epsilon_{\rm grav, X}\).

The final term reflects the change in internal energy due to changes in composition (at fixed density and temperature) and is referred to in MESA as eps_grav_composition_term. It is defined as

\(\epsilon_{\rm grav, X} \equiv -\sum_i \left(\frac{\partial e}{\partial X_i}\right)_{\rho,T, \{X\ne X_i\}} \frac{DX_i}{Dt}\),

and MESA evaluates this term using the finite difference

\(\epsilon_{\rm grav, X} = -\frac{1}{\delta t}\left[e(\rho, T, X) - e(\rho, T, X_{\rm start})\right]\),

where \(\delta t\) is the timestep and \(X_{\rm start}\) is the start-of-step mass fractions. (Other quantities take their end-of-step values.)

Note: In a phase transition, eps_grav includes the latent heat.

As with the dedt form, the error in numerical energy conservation (quantified by rel_E_err) reflects the energy equation residuals (i.e., the extent to which the energy equation was not satisfied). However, because this version of the energy equation is not written in a conservative form, it also includes error associated with the time discretization. An additional source of error enters because the equation of state provided by the eos module does not precisely satisfy the mathematical and thermodynamic identities that are used in rewriting the total and partial derivatives present in the equation. This inconsistency is usually worst at the conditions where MESA blends different component EOSes. It is important to understand that time discretization error and eos inconsistencies also affect models using the dedt form of the energy equation but manifest in different ways (e.g., as entropy generation). Under degenerate conditions, it is often preferable to incur energy errors rather than entropy errors, and the eps_grav form should generally be preferred in such circumstances.

In practice, the error sources usually exhibit the ordering (time discretization) > (eos inconsistency) >> (equation residuals). With increasing time resolution, the time discretization error can be driven down to the floor imposed by the eos inconsistency error. The value of this floor depends on the physical conditions, but may be \(\sim 10^{-4}\), well above the level of the residuals (\(\lesssim 10^{-8}\)). The control use_time_centered_eps_grav provides a time-centered implementation of eps_grav that can often reach this floor at larger timesteps. Convergence studies targeting the physical quantities of interest remain essential.

include_composition_in_eps_grav

If true, evaluate eps_grav_composition_term and include this quantity in eps_grav.

When this flag is true, the composition derivatives of eps_grav are also included in the Jacobian.

If this flag is set to false, the eps_grav form will not conserve energy in situations with changing composition.

include_composition_in_eps_grav = .true.

use_time_centered_eps_grav

If true, use a time-centered version of eps_grav and eps_grav_composition_term. (Disabled during relax.)

use_time_centered_eps_grav = .true.

Gamma_lnS_eps_grav_full_off

Gamma_lnS_eps_grav_full_on

Automatic switch to lnS form for eps_grav (\(\epsilon_{\rm grav} = -T\frac{Ds}{Dt}\)) in regions with high Gamma (plasma interaction parameter). These controls only apply when using the PC EOS. This is necessary to get the latent heat associated with the crystallization phase transition. The composition term \(-\sum_i (\partial e/\partial Y_i)_{s,\rho} dY_i\) is never included when the lnS form is used, independent of the setting of the control include_composition_in_eps_grav.

Gamma_lnS_eps_grav_full_on = 150d0
Gamma_lnS_eps_grav_full_off = 120d0

eps_grav_factor

multiply eps_grav by this factor

eps_grav_factor = 1d0

velocity_q_upper_bound

Local override for global v_flag. If local q > this bound, local v_flag is set false, else local v_flag is set to global v_flag. this lets you force v = 0 in outer envelope.

velocity_q_upper_bound = 1d99

velocity_tau_lower_bound

Local override for global v_flag. If local tau < this bound, local v_flag is set false, else local v_flag is set to global v_flag. this lets you force v = 0 in outer envelope.

velocity_tau_lower_bound = -1d99

velocity_logT_lower_bound

Local override for global v_flag. If local logT < this bound, local v_flag is set false, else local v_flag is set to global v_flag. this lets you force v = 0 in outer envelope.

velocity_logT_lower_bound = -1d99

max_dt_yrs_for_velocity_logT_lower_bound

Only apply velocity_logT_lower_bound when timestep < this limit.

max_dt_yrs_for_velocity_logT_lower_bound = 1d99

use_gravity_rotation_correction

With rotation, multiply gravity by fp_rot if this flag is true. See the 2nd MESA paper (2013), equation 22. previously called “use_dP_dm_rotation_correction”.

use_gravity_rotation_correction = .true.

non_nuc_neu_factor

Multiplies power from non-nuclear reaction neutrinos. i.e., thermal neutrinos such as computed by mesa/neu.

non_nuc_neu_factor = 1

eps_nuc_factor

Multiplies eps_nuc without changing rates or dxdt_nuc. Thus controls energy production without modifying the amount of change in abundances.

eps_nuc_factor = 1

eps_WD_sedimentation_factor

This controls energy production from sedimentation of Ne22 (and possibly other neutron-rich elements in WD interiors).

eps_WD_sedimentation_factor = 1

max_abs_eps_nuc

Limit magnitude of eps_nuc to this.

max_abs_eps_nuc = 1d99

fe56ec_fake_factor

min_T_for_fe56ec_fake_factor

Multiplier on ni56 electron capture rate to take isotopes in hardwired networks to more neutron rich isotopes.

fe56ec_fake_factor = 1d-7
min_T_for_fe56ec_fake_factor = 3d9

eps_mdot_factor

multiply eps_mdot by this factor

eps_mdot_factor = 1d0

max_num_surf_revisions

Max number of forced reconverges for changes in surf_lnS.

max_num_surf_revisions = 1

max_abs_rel_change_surf_lnS

Force solver reconverge if surf_lnS changed more than this.

max_abs_rel_change_surf_lnS = 5d-4

extra_power_source

erg/g/sec applied uniformly throughout the model This can be used to push a pre-ms model up the track to lower center temperatures. Can be used simultaneously with inject_extra_ergs_sec and inject_uniform_extra_heat

extra_power_source = 0

inject_uniform_extra_heat

extra heat in erg g^-1 s^-1 Added to cells in range min_q_for_uniform_extra_heat to max. Can be used simultaneously with inject_extra_ergs_sec and extra_power_source.

inject_uniform_extra_heat = 0

min_q_for_uniform_extra_heat

sets bottom of region for inject_uniform_extra_heat

min_q_for_uniform_extra_heat = 0

max_q_for_uniform_extra_heat

sets top of region for inject_uniform_extra_heat

max_q_for_uniform_extra_heat = 1

inject_extra_ergs_sec

added to mass equal to grams_for_inject_extra_core_ergs_sec can be used simultaneously with extra_power_source and inject_uniform_extra_heat

inject_extra_ergs_sec = 0

base_of_inject_extra_ergs_sec

(units: Msun) sets bottom of region for inject_extra_ergs_sec note: actual base is at max of this and the center of the model

base_of_inject_extra_ergs_sec = 0

total_mass_for_inject_extra_ergs_sec

(units: Msun) sets size of region for inject_extra_ergs_sec

total_mass_for_inject_extra_ergs_sec = 0

start_time_for_inject_extra_ergs_sec

(units: sec) start time for injecting extra ergs/s

start_time_for_inject_extra_ergs_sec = -1d99

duration_for_inject_extra_ergs_sec

(units: sec) length of time for injecting extra ergs/s set to negative value to keep injecting indefinitely or until reach target

duration_for_inject_extra_ergs_sec = -1

inject_until_reach_model_with_total_energy

(units: ergs) target for model total energy usually want to set duration_for_inject_extra_ergs_sec = -1 for this option. continue injecting until total energy of model reaches min of inject_until_reach_model_with_total_energy, and initial total energy

inject_until_reach_model_with_total_energy = 1d99

steps_before_use_velocity_time_centering

include_P_in_velocity_time_centering

include_L_in_velocity_time_centering

use_P_d_1_div_rho_form_of_work_when_time_centering_velocity

P_theta_for_velocity_time_centering

L_theta_for_velocity_time_centering

for time weighting in energy and momentum equations to give intrinsic conservation of total energy (conservation -> perfect as residuals -> 0), and to minimize numerical damping. as discussed in the 3rd mesa instrument paper (2015). time centering applies to velocities, pressures, and luminosities. not for u_flag. steps_before_use_velocity_time_centering < 0 means no time centering. P_theta and L_theta = 0.5 for time centered, = 1.0 for fully implicit.

steps_before_use_velocity_time_centering = -1
include_P_in_velocity_time_centering = .false.
P_theta_for_velocity_time_centering = 0.5d0
include_L_in_velocity_time_centering = .false.
L_theta_for_velocity_time_centering = 0.5d0
use_P_d_1_div_rho_form_of_work_when_time_centering_velocity = .false.

use_dPrad_dm_form_of_T_gradient_eqn

use_flux_limiting_with_dPrad_dm_form

use_gradT_actual_vs_gradT_MLT_for_T_gradient_eqn

These are for alternatives ways to determine the T gradient. The standard form of the equation is

dT/dm = dP/dm * T/P * grad_T, grad_T = dlnT/dlnP from MLT.

use hydrostatic value for dP/dm in this. this is because of limitations of MLT for calculating grad_T. (MLT assumes hydrostatic equilibrium) see comment in K&W chpt 9.1.

The alternatives forms are for dynamic situations where the use of hydrostatic dP/dm is inappropriate. In order of priority,

if (use_gradT_actual_vs_gradT_MLT_for_T_gradient_eqn)

equation is gradT(k)*(lnPeos(k-1) - lnPeos(k)) = lnT(k-1) - lnT(k)

recall that gradT(k) is expected dlnT/dlnPeos at face k from MLT.

if (use_dPrad_dm_form_of_T_gradient_eqn)

if (gradT < gradr) then

use L_rad = L*gradT/gradr (see, e.g., Cox&Giuli 14.109)

else

use L_rad = L

if (use_flux_limiting_with_dPrad_dm_form)

flxR = 4 * pi * r^2 * abs(dT^4/dm) / kap

flxLambda = (6 + 3*flxR) / (6 + 3*flxR + flxR^2) (see Levermore & Pomraning 1981)

L_rad = L_rad / flxLambda

With the resulting L_rad, determine the expected dT/dm by

d_Prad/dm = -kap*L_rad/(clight*area^2) – see, e.g., K&W (5.12)

use_dPrad_dm_form_of_T_gradient_eqn = .false.
use_flux_limiting_with_dPrad_dm_form = .false.
use_gradT_actual_vs_gradT_MLT_for_T_gradient_eqn = .false.

Hydrodynamic drag

drag_coefficient

min_q_for_drag

only when v_flag = .true.. Adjusts both v and energy transfer from kinetic to thermal. only for v(k) when q(k) > min_q_for_drag. kill off fraction of v = drag_coefficient (i.e. set to 1 to keep v near 0) useful for preventing the development radial pulsations during advanced burning in massive stars and AGB stars.

Under certain circumstances we will not have drag in the surface k=1 zone To force the drag term to be on in the outer zone you must enable one of the following surface boundary conditions: use_momentum_outer_BC, use_zero_Pgas_outer_BC, or use_fixed_Psurf_outer_BC

If use_drag_energy = .true. adds the work done by the drag force to the energy balance. Since the drag force is proportional to the velocity which is subject to numerical spikes and oscillations, you may not want to use the work done by it in the model If set to .false. but drag_coefficient is nonzero, the drag force will be applied in the momentum equation (as a numerical trick to damp spurious velocities) but not in the energy equation.

use_drag_energy = .true.
drag_coefficient = 0d0
min_q_for_drag = 0d0

v_drag_factor

v_drag

q_for_v_drag_full_off

q_for_v_drag_full_on

Only when u_flag = .true.. Adds a pseudo drag term of the form -v_drag_factor*(v-v_drag)^2/r, can be used damp velocities in outer layers of a star, useful for smoothing out spurious shocks colliding in ejected layers. Effect is full on for q>q_for_v_drag_full_on and full off for q < q_for_v_drag_full_off.

v_drag_factor = 0d0
v_drag = 0d0
q_for_v_drag_full_off = 0.95d0
q_for_v_drag_full_on = 0.96d0

Rayleigh-Taylor Instability: hydro drag terms

for hydro comparison tests (e.g., Sedov)

RTI_A

RTI_B

RTI_C

RTI_D

RTI_C_X_factor

RTI_C_X0

RTI_max_alpha

RTI_min_dm_behind_shock_for_full_on

RTI_dm_for_center_alpha_nondecreasing

RTI_energy_floor

RTI_D_mix_floor

RTI_min_m_for_D_mix_floor

RTI_log_max_boost

RTI_m_full_boost

RTI_m_no_boost

Note that these parameters are not exactly the same as used by Paul Duffell. His calibrated D is 2, where mesa has default D = 3 (see MESA IV). Users should try various values since the choice is not clear cut.

RTI_A = 1d-3
RTI_B = 2.5d0
RTI_C = 0.2d0
RTI_D = 3d0

RTI_C_X0_frac = 0.9d0
RTI_C_X_factor = 0d0

RTI_max_alpha = 0.5d0
RTI_min_dm_behind_shock_for_full_on = 0d0
RTI_dm_for_center_eta_nondecreasing = 0.02d0
RTI_energy_floor = 0d0
RTI_D_mix_floor = 0d0
RTI_min_m_for_D_mix_floor = 0d0

RTI_log_max_boost = 3d0
RTI_m_full_boost = 4d0
RTI_m_no_boost = 5d0

retry_for_v_above_clight

If .true., a retry will be triggered at the end of a step if the maximum velocity exceeds the speed of light. If .false., only a warning is printed.

retry_for_v_above_clight = .true.

solver controls

the following is from a response on mesa-users to a question about controls for solver tolerances:

The “residual” is the left over difference between the left and right hand sides of the equation we are trying to solve. We do iterations to reduce that, but we are limited by the non-linearity of the problem and the quality of the estimates for the derivatives.

The “correction” is the change in the primary variable that is calculated using good-old Newton’s rule in multiple dimensions — so Jacobian and residuals give a correction that would make the next residual vanish if the problem were linear and the Jacobian was exact, neither of which are true. So the best we can hope for is that the corrections will get smaller next time.

The “norm” is the average; the “max” is the max. Sometimes you mainly care about the norm and will accept a few outliers. But sometimes you don’t want any really bad outliers, so you want to set a low limit for the max residual or correction as well as the norm.

You might want to try for several iterations with strict tolerances, and then relax them if things are still not converged. For example, you might be willing to live with the larger tolerances, but you’d like to give it a good try at the smaller ones before switching. Also, you might be willing to settle for any-old residual if the corrections have become small enough. You can do that too by relaxing the residual tolerances after a few iterations.

Hope that at least helps with the nomenclature.

I agree with Frank that you should consider the effects of smaller timesteps and more grid points as your main technique — tightening up the tolerances for the solver won’t help if you are taking timesteps that are too large or if you have inadequate grid resolution.

tol_correction_norm

tol_max_correction

“Correction” for variable x(i,k) is scaled change, dx(i,k)/xscale(i,k). these tolerances are for the magnitude of the scaled corrections.

tol_correction_norm = 3d-5
tol_max_correction = 3d-3

tol_correction_high_T_limit

For very late stages of massive star evolution, need to relax tolerances. If max T >= this limit, switch scaling factors.

tol_correction_high_T_limit = 1d9

tol_correction_norm_high_T

tol_max_correction_high_T

Above tol_correction_high_T_limit use these scaling factors.

tol_correction_norm_high_T = 3d-3
tol_max_correction_high_T = 3d-1

tol_correction_extreme_T_limit

For very late stages of massive star evolution, need to relax tolerances. If center T >= this limit, switch scaling factors.

tol_correction_extreme_T_limit = 6d9

tol_correction_norm_extreme_T

tol_max_correction_extreme_T

For very late stages of massive star evolution, need to relax tolerances. If center T >= this limit, switch scaling factors.

tol_correction_norm_extreme_T = 8d-3
tol_max_correction_extreme_T = 8d-1

tol_bad_max_correction

if max_correction > tol_max_correction and no more iterations allowed, then still accept the solution if max_correction <= tol_bad_max_correction. but if max_correction > tol_bad_max_correction, then reject the solution.

tol_bad_max_correction = 0d0

bad_max_correction_series_limit

If have this many steps in a row with max_correction > tol_max_correction, then do a retry with a smaller timestep.

bad_max_correction_series_limit = 2

relax_use_gold_tolerances

relax_use_gold_tolerances = .false.

relax_solver_iters_timestep_limit

relax_tol_correction_norm

relax_tol_max_correction

relax_tol_residual_norm1

relax_tol_max_residual1

relax_iter_for_resid_tol2

relax_tol_residual_norm2

relax_tol_max_residual2

relax_iter_for_resid_tol3

relax_tol_residual_norm3

relax_tol_max_residual3

relax_maxT_for_gold_tolerances

For use during relax operations. Only used if /= 0.

relax_solver_iters_timestep_limit = 0

relax_tol_correction_norm = 0d0
relax_tol_max_correction = 0d0

relax_tol_residual_norm1 = 0d0
relax_tol_max_residual1 = 0d0
relax_iter_for_resid_tol2 = 3

relax_tol_residual_norm2 = 0d0
relax_tol_max_residual2 = 0d0
relax_iter_for_resid_tol3 = 0

relax_tol_residual_norm3 = 0d0
relax_tol_max_residual3 = 0d0
relax_maxT_for_gold_tolerances = -1d0

include_L_in_correction_limits

include_v_in_correction_limits

include_u_in_correction_limits

include_w_in_correction_limits

These variables can be excluded from calculation of correction norm and max.

include_L_in_correction_limits = .true.
include_v_in_correction_limits = .true.
include_u_in_correction_limits = .true.
include_w_in_correction_limits = .true.

max_X_for_conv_timescale

min_X_for_conv_timescale

max_q_for_conv_timescale

min_q_for_conv_timescale

max_q_for_QHSE_timescale

min_q_for_QHSE_timescale

max_X_for_conv_timescale = 1d0
min_X_for_conv_timescale = 0d0
max_q_for_conv_timescale = 1d0
min_q_for_conv_timescale = 0d0
max_q_for_QHSE_timescale = 1d0
min_q_for_QHSE_timescale = 0d0

correction_xa_limit

Ignore correction to abundance when calculating correction norm and max if current mass fraction is less than this limit.

correction_xa_limit = 5d-3

xa_scale

Scaling for abundance variables is max(xa_scale, current mass fraction).

xa_scale = 1d-5

tol_residual_norm1

tol_max_residual1

iter_for_resid_tol2

“residual” for equation is the difference between left and right sides use tol_residual_norm1 & tol_max_residual1 at iteration number iter_for_resid_tol2, switch to next tolerances.

tol_residual_norm1 = 1d-10
tol_max_residual1 = 1d-9
iter_for_resid_tol2 = 6

tol_residual_norm2

tol_max_residual2

iter_for_resid_tol3

Use tol_residual_norm2 & tol_max_residual2 these apply starting at iteration number iter_for_resid_tol2. at iteration number iter_for_resid_tol3, switch to next tolerances.

tol_residual_norm2 = 1d90
tol_max_residual2 = 1d90
iter_for_resid_tol3 = 15

tol_residual_norm3

tol_max_residual3

Use tol_residual_norm3 & tol_max_residual3 these apply starting at iteration number iter_for_resid_tol3.

tol_residual_norm3 = 1d90
tol_max_residual3 = 1d90

If things get worse from one iteration to next, give up. The following are the limits that define “getting worse enough to stop”.

corr_norm_jump_limit

If correction norm increases by this factor or more, quit.

corr_norm_jump_limit = 1d99

max_corr_jump_limit

If correction max increases by this factor or more, quit.

max_corr_jump_limit = 1d6

resid_norm_jump_limit

If residual norm increases by this factor or more, quit.

resid_norm_jump_limit = 1d99

max_resid_jump_limit

If residual max increases by this factor or more, quit.

max_resid_jump_limit = 1d6

convergence_ignore_equL_residuals

convergence_ignore_equL_residuals = .false.

convergence_ignore_alpha_RTI_residuals

convergence_ignore_alpha_RTI_residuals = .false.

trace_solver_damping

Send solver damping data to screen.

trace_solver_damping = .false.

do_normalize_dqs_as_part_of_set_qs

normalize_dqs destroys bit-for-bit read as inverse of write for models. ok for create pre ms etc., but not for read model create_pre_ms calls normalize_dqs even if this flag is false.

do_normalize_dqs_as_part_of_set_qs = .false.

use_DGESVX_in_bcyclic use_equilibration_in_DGESVX report_min_rcond_from_DGESXV

FOR DEBUGGING ONLY. NOT FOR GENERAL USE.

use_DGESVX_in_bcyclic = .false.
use_equilibration_in_DGESVX = .false.
report_min_rcond_from_DGESXV = .false.

solver_max_tries_before_reject

Max number solver iterations before give up.

solver_max_tries_before_reject = 25

max_tries1

Max tries on 1st model.

max_tries1 = 250

max_tries_for_retry

Normal number of retries.

max_tries_for_retry = 25

max_tries_after_5_retries

Increase number of tries after 5 failed ones.

max_tries_after_5_retries = 35

max_tries_after_10_retries

Increase number of tries after 10 failed ones.

max_tries_after_10_retries = 50

max_tries_after_20_retries

Increase number of tries after 20 failed ones.

max_tries_after_20_retries = 75

retry_limit

Only use if > 0. In case the solver fails for some reason, it will retry with a smaller timestep. It does up to this many retries for the current step before terminating.

retry_limit = 100

redo_limit

Only use if > 0. Do up to this many redo’s for the current step before terminating.

redo_limit = 100

solver_itermin

Use at least this many iterations in solver for hydro solve.

solver_itermin = 2

solver_itermin_until_reduce_min_corr_coeff

Use at least this many iterations in solver before try using small min_corr_coeff

solver_itermin_until_reduce_min_corr_coeff = 8

solver_reduced_min_corr_coeff

For use with solver_itermin_for_reduce_min_corr_coeff.

solver_reduced_min_corr_coeff = 0.1d0

tiny_corr_coeff_limit

scale_correction_norm

corr_param_factor

scale_max_correction

ignore_too_large_correction

corr_coeff_limit

tiny_corr_factor

ignore_min_corr_coeff_for_scale_max_correction

ignore_species_in_max_correction

num_times_solver_reuse_mtx

see star/private/star_solver for info about these

tiny_corr_coeff_limit = 100
scale_correction_norm = 0.1d0
corr_param_factor = 10
scale_max_correction = 1d99
ignore_too_large_correction = .false.
corr_coeff_limit = 1d-2
tiny_corr_factor = 2
ignore_min_corr_coeff_for_scale_max_correction = .false.
ignore_species_in_max_correction = .false.
num_times_solver_reuse_mtx = 0

min_xa_hard_limit

min_xa_hard_limit_for_highT

If solver produces mass fraction < this limit, then reject the trial solution. Can optionally relax this limit at high T.

min_xa_hard_limit = -1d-5
min_xa_hard_limit_for_highT = -3d-5

logT_max_for_xa_hard_limit

Use min_xa_hard_limit for center logT <= this.

logT_max_for_min_xa_hard_limit = 9.49d0

logT_min_for_xa_hard_limit_for_highT

Use min_xa_hard_limit_for_highT for center logT >= this. Linear interpolate in logT for intermediate center temperatures.

logT_min_for_min_xa_hard_limit_for_highT = 9.51d0

sum_xa_hard_limit

sum_xa_hard_limit_for_highT

If solver produces any cell with abs(sum(xa)-1) > this limit, then reject the trial solution. Can optionally relax this limit at high T.

sum_xa_hard_limit = 5d-4
sum_xa_hard_limit_for_highT = 1d-3

logT_max_for_sum_xa_hard_limit

Use sum_xa_hard_limit for center logT <= this.

logT_max_for_sum_xa_hard_limit = 9.40d0

logT_min_for_sum_xa_hard_limit_for_highT

Use sum_xa_hard_limit_for_highT for center logT >= this. Linear interpolate in logT for intermediate center temperatures.

logT_min_for_sum_xa_hard_limit_for_highT = 9.44d0

do_solver_damping_for_neg_xa

If true, uniformly reduce solver corrections if necessary to avoid neg abundances.

do_solver_damping_for_neg_xa = .true.

scale_max_correction_for_negative_surf_lum

max_frac_for_negative_surf_lum

If true, then scales the correction factor in a Newton iteration to prevent the surface from reaching a negative luminosity. If an iteration would require s% L(1) to become negative, then the correction is scaled such that the change in surface luminosity is -max_frac_for_negative_surf_lum*s% L(1)

scale_max_correction_for_negative_surf_lum = .false.
max_frac_for_negative_surf_lum = 0.8

min_chem_eqn_scale

min_chem_eqn_scale = 1d0

hydro_mtx_max_allowed_{abs}{dlogT | dlogRho | logT | logRho}

Force retry with smaller timestep if hydro solves change T or Rho by too much or make them too large.

hydro_mtx_max_allowed_abs_dlogT = 99d0
hydro_mtx_max_allowed_abs_dlogRho = 99d0
min_logT_for_hydro_mtx_max_allowed = -1d99
hydro_mtx_max_allowed_logT = 12d0
hydro_mtx_max_allowed_logRho = 12d0

hydro_mtx_min_allowed_logT = 1d0
hydro_mtx_min_allowed_logRho = -1d2

level 1 of gold tolerances for solver solver

use_gold_tolerances

steps_before_use_gold_tolerances

gold_solver_iters_timestep_limit

maxT_for_gold_tolerances

gold_tol_residual_norm1

gold_iter_for_resid_tol2

gold_tol_residual_norm2

gold_tol_max_residual2

gold_iter_for_resid_tol3

gold_tol_residual_norm3

gold_tol_max_residual3

use_gold_tolerances = .true.
steps_before_use_gold_tolerances = -1

if >= 0, then after this many steps in run, act as if use_gold_tolerances true this allows a delay before turning on gold tolerances NOTE: if using steps_before_use_gold_tolerances >= 0, then set use_gold_tolerances = false

maxT_for_gold_tolerances = 1d99

gold_tol_residual_norm1 = 1d-11
gold_tol_max_residual1 = 1d-9
gold_iter_for_resid_tol2 = 5
gold_tol_residual_norm2 = 1d-8
gold_tol_max_residual2 = 1d-6
gold_iter_for_resid_tol3 = 10
gold_tol_residual_norm3 = 1d-6
gold_tol_max_residual3 = 1d-4

gold_solver_iters_timestep_limit = 14

level 2 of gold tolerances for solver solver - tighter than level 1

use_gold2_tolerances

steps_before_use_gold2_tolerances

gold2_solver_iters_timestep_limit

gold2_tol_residual_norm1

gold2_iter_for_resid_tol2

gold2_tol_residual_norm2

gold2_tol_max_residual2

gold2_iter_for_resid_tol3

gold2_tol_residual_norm3

gold2_tol_max_residual3

use_gold2_tolerances = .false.
steps_before_use_gold2_tolerances = -1

if >= 0, then after this many steps in run, act as if use_gold2_tolerances true this allows a delay before turning on level 2 gold tolerances NOTE: if using steps_before_use_gold2_tolerances >= 0, then set use_gold2_tolerances = false

gold2_tol_residual_norm1 = 1d-11
gold2_tol_max_residual1 = 1d-9
gold2_iter_for_resid_tol2 = 5
gold2_tol_residual_norm2 = 1d-10
gold2_tol_max_residual2 = 1d-8
gold2_iter_for_resid_tol3 = 10
gold2_tol_residual_norm3 = 1d-8
gold2_tol_max_residual3 = 1d-5

gold2_solver_iters_timestep_limit = 18

include_rotation_in_total_energy

previously called include_rotation_in_energy_error_report

include_rotation_in_total_energy = .false.

artificial viscosity

use_Pvsc_art_visc

Pvsc_cq

Pvsc_zsh

Pvsc is artificial pressure to push back against compression this is the form of artificial viscosity used in RSP if using this, do not set use_artificial_viscosity true.

artificial viscosity controls for the equations see: Appendix C in Stellingwerf 1975 http://adsabs.harvard.edu/abs/1975ApJ…195..441S. In principle, for not too-non-adiabatic convective models artificial viscosity is not needed or should be very small. Hence a large cut-off parameter below (in purely radiative models the default value for cut-off was 0.01)

zsh > 0 delays onset of artificial viscosity can eliminate most/all interior dissipation while still providing for extreme cases. using this parameter the dependence of limiting amplitude on cq is very weak.

use_Pvsc_art_visc = .false.
Pvsc_cq = 4.0d0
Pvsc_zsh = 0.1d0

use_artificial_viscosity

use_artificial_viscosity has been replaced by use_Pvsc_art_visc.

split burn

op_split_burn

op_split_burn = .false.

op_split_burn_min_T

op_split_burn_eps

op_split_burn_odescal

Only do op_split_burn in cells with T >= this limit at start of step.

op_split_burn_min_T = 2d9
op_split_burn_eps = 1d-5
op_split_burn_odescal = 1d-5

op_split_burn_eps_nuc_infall_limit

turn off op_split_burn nuclear burning if max infall speed exceeds this limit (cm/s).

op_split_burn_eps_nuc_infall_limit = 1d99

timestep controls

The terminal output during evolution includes a short string for the dt_limit. This is to give you some indication of what is limiting the time steps. Here’s a dictionary mapping those terminal strings to the corresponding control parameters. (There is a similar table in mesa/binary/defaults/binary_controls.defaults.)

 terminal output       related parameter
'burn steps'           burn_steps_limit
'Lnuc'                 delta_lgL_nuc_limit
'Lnuc_cat'             delta_lgL_nuc_cat_limit
'Lnuc_H'               delta_lgL_H_limit
'Lnuc_He'              delta_lgL_He_limit
'lgL_power_phot'       delta_lgL_power_photo_limit
'Lnuc_z'               delta_lgL_z_limit
'bad_X_sum'            (solver found bad mass sum)
'dL/L'                 dL_div_L_limit
'dX'                   dX_limit
'dX/X'                 dX_div_X_limit
'dX_nuc_drop'          dX_nuc_drop_limit
'delta mdot'           delta_mdot_limit
'delta total J'        delta_lg_total_J_limit
'delta_HR'             delta_HR_limit
'delta_mstar'          delta_lg_star_mass_limit
'diff iters'           diffusion_iters_limit
'diff steps'           diffusion_steps_limit
'min_dr_div_cs'        dt_div_min_dr_div_cs_limit
'dt_collapse'          dt_div_dt_cell_collapse_limit
'eps_nuc_cntr'         delta_log_eps_nuc_cntr_limit
'error rate'           limit_for_log_rel_rate_in_energy_conservation
'highT del Ye'         delta_Ye_highT_limit
'hold'                 (recent retry, so no increase in dt)
'lgL'                  delta_lgL_limit
'lgP'                  delta_lgP_limit
'lgP_cntr'             delta_lgP_cntr_limit
'lgR'                  delta_lgR_limit
'lgRho'                delta_lgRho_limit
'lgRho_cntr'           delta_lgRho_cntr_limit
'lgT'                  delta_lgT_limit
'lgT_cntr'             delta_lgT_cntr_limit
'lgT_max'              delta_lgT_max_limit
'lgT_max_hi_T'         delta_lgT_max_at_high_T_limit
'lgTeff'               delta_lgTeff_limit
'dX_div_X_cntr'        delta_dX_div_X_cntr_limit
'lg_XC_cntr'           delta_lg_XC_cntr_limit
'lg_XH_cntr'           delta_lg_XH_cntr_limit
'lg_XHe_cntr'          delta_lg_XHe_cntr_limit
'lg_XNe_cntr'          delta_lg_XNe_cntr_limit
'lg_XO_cntr'           delta_lg_XO_cntr_limit
'lg_XSi_cntr'          delta_lg_XSi_cntr_limit
'XC_cntr'              delta_XC_cntr_limit
'XH_cntr'              delta_XH_cntr_limit
'XHe_cntr'             delta_XHe_cntr_limit
'XNe_cntr'             delta_XNe_cntr_limit
'XO_cntr'              delta_XO_cntr_limit
'XSi_cntr'             delta_XSi_cntr_limit
'log_eps_nuc'          delta_log_eps_nuc_limit
'max_dt'               max_years_for_timestep
'neg_mass_frac'        (solver found neg mass frac)
'adjust_J_q'           adjust_J_q_limit
'solver iters'         solver_iters_timestep_limit
'rel_E_err'            limit_for_rel_error_in_energy_conservation
'varcontrol'           varcontrol_target
'max increase'         max_timestep_factor or max_timestep_factor_at_high_T
'max decrease'         min_timestep_factor
'retry'                (just did a retry)
'b_****'               see binary/defaults/binary_controls.defaults

time_delta_coeff

time_delta_coeff - smaller forces smaller timesteps giving better time resolution. multiplier for all real number timestep limits and hard limits. does not apply to integer valued limits such as

• solver_iters_timestep_limit

• burn_steps_limit

• diffusion_steps_limit

• diffusion_iters_limit

does not apply to varcontrol_target. analogous to mesh_delta_coeff for better spatial resolution.

time_delta_coeff = 1d0

max_timestep

In seconds. max_timestep <= 0 means no upper limit.

max_timestep = 0

max_years_for_timestep

max_years_for_timestep <= 0 means no upper limit. Note: max_timestep is the control that is used by most of the code. max_years_for_timestep is just provided as a convenience. At the start of each step, the evolve routine checks to see if max_years_for_timestep > 0, and if so, it sets max_timestep = max_years_for_timestep*secyer.

max_years_for_timestep = 0

max_timestep_hi_T_limit

If max T >= this, then switch to hi_T_max_years_for_timestep. Ignore if <= 0.

max_timestep_hi_T_limit = -1

hi_T_max_years_for_timestep

Max years for timestep if max_timestep_hi_T_limit is active.

hi_T_max_years_for_timestep = 0

min_timestep_factor

Lower limit for ratio of new timestep to previous timestep. i.e., allow dt to get smaller by no more than this factor – 0 means no limit.

min_timestep_factor = 0.8d0

force_timestep

In seconds. force_timestep <= 0 means no forced timestep.

force_timestep = 0

force_timestep_years

Note: force_timestep is the control that is used by most of the code. force_timestep_years is just provided as a convenience. At the start of each step, the evolve routine checks if force_timestep_years > 0, and if so, it sets force_timestep = force_timestep_years*secyer.

force_timestep_years = 0

force_timestep_min

In seconds. force_timestep_min <= 0 means no forced lower limit.

force_timestep_min = 0

force_timestep_min_years

Note: force_timestep_min is the control that is used by most of the code. force_timestep_min_years is just provided as a convenience. At the start of each step, the evolve routine checks if force_timestep_min_years > 0, and if so, it sets force_timestep_min = force_timestep_min_years*secyer.

force_timestep_min_years = 0

force_timestep_min_factor

If dt is < force_timestep_min, then replace dt by min(dt*force_timestep_min_factor, force_timestep_min)

force_timestep_min_factor = 2d0

max_timestep_factor

max_timestep_factor_at_high_T

min_logT_for_max_timestep_factor_at_high_T

Upper limit for ratio of new timestep to previous timestep. i.e., allow dt to get larger by no more than this factor – 0 means no limit. use max_timestep_factor_at_high_T when max logT > min_logT_for_max_timestep_factor_at_high_T.

max_timestep_factor = 1.2d0
max_timestep_factor_at_high_T = 1.1d0
min_logT_for_max_timestep_factor_at_high_T = 1d99

timestep_factor_for_retries

Before retry, decrease dt by this.

timestep_factor_for_retries = 0.5d0

retry_hold

No increases in timestep for retry_hold steps after a retry.

retry_hold = 1

neg_mass_fraction_hold

No increases in timestep for neg_mass_fraction_hold steps after a retry caused by a negative mass fraction.

neg_mass_fraction_hold = 2

timestep_dt_factor = 0.9

dt reduction factor exceed timestep limits.

timestep_dt_factor = 0.9d0

use_dt_low_pass_controller

Enable low pass filter for smoother timestep variations.

use_dt_low_pass_controller = .true.

varcontrol_target

This is the target value for relative variation in the structure from one model to the next. The default timestep adjustment is to increase or reduce the timestep depending on whether the actual variation was smaller or greater than this value.

varcontrol_target = 1d-3

min_allowed_varcontrol_target

The run will terminate if varcontrol_target < min_allowed_varcontrol_target It is not usually a good idea to reduce this. Instead, use time_delta_coeff to do time resolution convergence studies.

min_allowed_varcontrol_target = 1d-4

varcontrol_dt_limit_ratio_hard_max

varcontrol_dt_limit_ratio is the actual varcontrol value divided by the target. if that ratio exceeds this limit, then retry with a smaller timestep. this let’s you prevent large changes from happening in a single step.

varcontrol_dt_limit_ratio_hard_max = 1d99

never_skip_hard_limits

If true, then don’t skip hard limits even immediately after a retry.

never_skip_hard_limits = .true.

relax_hard_limits_after_retry

If true, then don’t enforce hard limits immediately after a retry.

relax_hard_limits_after_retry = .false.

limits based on iterations required by various solvers

solver_iters_timestep_limit

If solver solve uses more solver_iterations than this, reduce the next timestep. NOTE: when using gold tolerances, set gold_solver_iters_timestep_limit.

solver_iters_timestep_limit = 7

burn_steps_limit

If burn solver uses more steps than this, reduce the next timestep.

burn_steps_limit = 10000

burn_steps_hard_limit

If burn solver uses more steps than this, retry.

burn_steps_hard_limit = 20000

diffusion_steps_limit

If diffusion solver uses more steps than this, reduce the next timestep.

diffusion_steps_limit = 500

diffusion_steps_hard_limit

If diffusion solver uses more steps than this, retry.

diffusion_steps_hard_limit = 700

diffusion_iters_limit

If use a total number of iters > this, reduce the next timestep.

diffusion_iters_limit = 600

diffusion_iters_hard_limit

If use a total number of iters > this, retry.

diffusion_iters_hard_limit = 800

limits based on max decrease in mass fraction at any location in star

dX_mix_dist_limit

Option to ignore decreases in abundance in non-mixed cells near mixing boundaries. Ignore abundance changes if nearest mixing boundary is closer than this in Msun units. This applies to dX, and dX_div_X limits.

dX_mix_dist_limit = 1d-4

dX_limit_species

Specify which species the dX_limit, dX_div_X_limit, etc array entries apply to. These are limits on magnitude of decrease in any cell abundance during a single timestep. dX here is abs(xa(j,k) - xa_old(j,k)) for any cell k and all species j, eg 'h1', 'he4', etc. Special ‘species’ 'X' (any hydrogen), 'Y' (any helium) and 'Z' (any metals) are allowed here. E.g. 'Z' will trigger the timestep control if any metal isotope abundance individually satisfies the conditions below. Considers all cells except where have convective mixing.

dX_limit_species(1) = 'h1'
dX_limit_species(2) = 'he4'
dX_limit_species(3:) = ''

dX_limit_min_X

dX limits only apply where xa(j,k) >= this limit.

dX_limit_min_X(:) = 1d99

dX_limit

If max dX is greater than this, reduce the next timestep by dX_limit/max_dX.

dX_limit(:) = 1d99

dX_hard_limit

If max dX is greater than this, retry with smaller timestep.

dX_hard_limit(:) = 1d99

dX_decreases_only

If true, then only consider decreases in abundance. dX_decreases_only applies to dX_div_X also.

dX_decreases_only(:) = .true.

Limit on magnitude of relative decrease in any cell abundance. dX_div_X here is abs(xa(j,k) - xa_old(j,k))/xa(j,k) for any cell k and any species j. Considers all cells except where have convective mixing.

dX_div_X_limit_min_X

dX_div_X limits only apply where xa(j,k) >= this limit.

dX_div_X_limit_min_X(1) = 1d-3
dX_div_X_limit_min_X(2) = 1d-3
dX_div_X_limit_min_X(3:) = 1d99

dX_div_X_limit

If max dX_div_X is greater than this, reduce the next timestep by dX_limit/max_dX.

dX_div_X_limit(1) = 0.9d0
dX_div_X_limit(2) = 0.9d0
dX_div_X_limit(3:) = 1d99

dX_div_X_hard_limit

If max dX_div_X is greater than this, retry with smaller timestep.

dX_div_X_hard_limit(:) = 1d99

dX_div_X_at_high_T_limit

dX_div_X_at_high_T_hard_limit

dX_div_X_at_high_T_limit_lgT_min

dX_div_X_at_high_T_limit(:) = 1d99
dX_div_X_at_high_T_hard_limit(:) = 1d99
dX_div_X_at_high_T_limit_lgT_min(:) = 1d99

Limits on max drop in abundance mass fraction from burning with possible mixing inflow. This considers both nuclear reactions and offsetting effect of mixing inflow.

dX_nuc_drop_min_X_limit

dX_nuc_drop_limit only for X > dX_nuc_drop_min_X_limit. note that this is the abundance of the species, not the H1 abundance for the cell. i.e., if species abundance is below this limit, then ignore it for the dX_nuc_drop limit.

dX_nuc_drop_min_X_limit = 1d-4

dX_nuc_drop_max_A_limit

dX_nuc_drop_limit only for species with A <= dX_nuc_drop_max_A_limit.

dX_nuc_drop_max_A_limit = 52

dX_nuc_drop_limit_at_high_T

Negative means use value for dX_nuc_drop_limit, else use this limit when max logT > 9.45.

dX_nuc_drop_limit_at_high_T = -1

dX_nuc_drop_limit

If max dX_nuc_drop is greater than dX_nuc_drop_limit, reduce the next timestep by dX_nuc_drop_limit/max_dX_nuc_drop.

dX_nuc_drop_limit = 5d-2

dX_nuc_drop_hard_limit

If max dX_nuc_drop is greater than dX_nuc_drop_hard_limit, retry with smaller timestep.

dX_nuc_drop_hard_limit = 1d99

dX_nuc_drop_min_yrs_for_dt

Don’t let dX_nuc_drop change dt to smaller than this.

dX_nuc_drop_min_yrs_for_dt = 1d-9

limits based on relative changes in variables L, P, Rho, T, R, eps_nuc

limit on magnitude of relative change in L at any grid point

dL_div_L = abs(L(k) - L_old(k))/L(k)

dL_div_L_limit

If max abs dL_div_L is greater than this, reduce the next timestep.

dL_div_L_limit = -1

dL_div_L_hard_limit

If max abs dL_div_L is greater than this, retry with smaller timestep.

dL_div_L_hard_limit = -1

dL_div_L_limit_min_L

In Lsun units. dL_div_L limits only apply where L(k) >= Lsun*dL_limit_min_L

dL_div_L_limit_min_L = 1d99

delta_lgP_limit

Limit for magnitude of max change in log10 total pressure in any cell.

delta_lgP_limit = 1

delta_lgP_hard_limit

If max delta_lgP is greater than delta_lgP_hard_limit, retry with smaller timestep.

delta_lgP_hard_limit = -1

delta_lgP_limit_min_lgP

delta_lgP_limit limits only apply where log10_P(k) >= delta_lgP_limit_min_lgP

delta_lgP_limit_min_lgP = 1d99

delta_lgRho_limit

Limit for magnitude of max change in log10 density in any cell.

delta_lgRho_limit = 1

delta_lgRho_hard_limit = -1

If max delta_lgRho is greater than delta_lgRho_hard_limit, retry with smaller timestep.

delta_lgRho_hard_limit = -1

delta_lgRho_limit_min_lgRho

delta_lgRho_limit limits only apply where log10_Rho(k) >= delta_lgRho_limit_min_lgRho.

delta_lgRho_limit_min_lgRho = 1d99

delta_lgT_limit

Limit for magnitude of max change in log10 temperature in any cell.

delta_lgT_limit = 0.5d0

delta_lgT_hard_limit

If max delta_lgT is greater than delta_lgT_hard_limit, retry with smaller timestep.

delta_lgT_hard_limit = -1

delta_lgT_limit_min_lgT

delta_lgT_limit limits only apply where log10_T(k) >= delta_lgT_limit_min_lgT.

delta_lgT_limit_min_lgT = 1d99

delta_lgE_limit

Limit for magnitude of max change in log10 internal energy in any cell.

delta_lgE_limit = 0.1d0

delta_lgE_hard_limit

If max delta_lgE is greater than delta_lgE_hard_limit, retry with smaller timestep.

delta_lgE_hard_limit = -1

delta_lgE_limit_min_lgE

delta_lgE_limit limits only apply where log10(E(k)) >= delta_lgE_limit_min_lgE.

delta_lgE_limit_min_lgE = 1d99

delta_lgR_limit

Limit for magnitude of max change in log10 radius at any cell boundary.

delta_lgR_limit = 0.5d0

delta_lgR_hard_limit

If max delta_lgR is greater than delta_lgR_hard_limit, retry with smaller timestep.

delta_lgR_hard_limit = -1

delta_lgR_limit_min_lgR

delta_lgR_limit limits only apply where log10_R(k) >= delta_lgR_limit_min_lgR.

delta_lgR_limit_min_lgR = 1d99

delta_Ye_highT_limit

Limit for magnitude of max change in Ye in high T cells.

delta_Ye_highT_limit = 99

Limit testing for max delta_ye to cells with T >= minT_for_highT_Ye_limit If this high T max delta_Ye is greater than delta_Ye_highT_limit, reduce the next timestep by delta_Ye_highT_limit/max_delta_Ye.

delta_Ye_highT_hard_limit = -1

minT_for_highT_Ye_limit

Limit testing for max delta_ye to cells with T >= minT_for_highT_Ye_limit. If this high T max delta_Ye is greater than delta_Ye_highT_limit, retry with smaller timestep.

minT_for_highT_Ye_limit = 7d9

delta_log_eps_nuc_limit

Limit for magnitude of max change in log10 eps_nuc in any cell. Only applies to increases in non-convective zones.

delta_log_eps_nuc_limit = -1

delta_log_eps_nuc_hard_limit

If max delta_log_eps_nuc is greater than delta_log_eps_nuc_hard_limit, retry with smaller timestep.

delta_log_eps_nuc_hard_limit = -1

limits based on integrated power at each point for each category of nuclear reaction

lgL_nuc_cat = nuclear reaction energy release for a particular category of reaction (Lsun units). Energy release here excludes neutrinos.

delta_lgL_nuc_cat_limit

Limit for magnitude of change in lgL_nuc for category.

delta_lgL_nuc_cat_limit = -1

delta_lgL_nuc_cat_hard_limit

If max delta is greater than delta_lgL_nuc_cat_hard_limit, retry with smaller timestep.

delta_lgL_nuc_cat_hard_limit = -1

lgL_nuc_cat_burn_min

Ignore changes in lgL_nuc for category if value is less than this.

lgL_nuc_cat_burn_min = -1

lgL_nuc_mix_dist_limit

Ignore if nearest boundary is closer than this. Ignore changes in lgL in cells near mixing boundaries.

lgL_nuc_mix_dist_limit = 1d-6

L_H_burn = integrated power at surface from PP and CNO (in Lsun units)

values for lgL_H are log10(max(1, L_H_burn))

delta_lgL_H_limit

limit for magnitude of change in lgL_H

delta_lgL_H_limit = -1

delta_lgL_H_hard_limit

if max delta is greater than delta_lgL_H_hard_limit, retry with smaller timestep

delta_lgL_H_hard_limit = -1

lgL_H_burn_min

ignore changes in lgL_H if value is less than this

lgL_H_burn_min = 1.5d0

lgL_H_drop_factor

when L_H is dropping, multiply limits by this factor

lgL_H_drop_factor = 1

lgL_H_burn_relative_limit

ignore changes in lgL_H if max(lgL_He,lgL_z) - lgL_H > this

lgL_H_burn_relative_limit = 3

L_He_burn = integrated power at surface from triple alpha (in Lsun units)

values for lgL_He are log10(max(1, L_He_burn))

delta_lgL_He_limit

Limit for magnitude of change in lgL_He.

delta_lgL_He_limit = 0.025d0

delta_lgL_He_hard_limit

If max delta is greater than delta_lgL_He_hard_limit, retry with smaller timestep.

delta_lgL_He_hard_limit = -1

lgL_He_burn_min

Ignore changes in lgL_He if value is less than this.

lgL_He_burn_min = 2.5d0

lgL_He_drop_factor

When L_He is dropping, multiply limits by this factor.

lgL_He_drop_factor = 1

lgL_He_burn_relative_limit

Ignore changes in lgL_He if max(lgL_H,lgL_z) - lgL_He > this.

lgL_He_burn_relative_limit = 3

L_z_burn = integrated power at surface from nuclear burning other than H, He, or C (in Lsun units) excluding photodistintegrations

values for lgL_z are log10(max(1, L_z_burn))

delta_lgL_z_limit

Limit for magnitude of change in lgL_z.

delta_lgL_z_limit = -1

delta_lgL_z_hard_limit

If max delta is greater than delta_lgL_z_hard_limit, retry with smaller timestep.

delta_lgL_z_hard_limit = -1

lgL_z_burn_min

Ignore changes in lgL_z if value is less than this.

lgL_z_burn_min = 2.5d0

lgL_z_drop_factor

When L_z is dropping, multiply limits by this factor.

lgL_z_drop_factor = 1

lgL_z_burn_relative_limit

Ignore changes in lgL_z if max(lgL_H,lgL_He) - lgL_z > this.

lgL_z_burn_relative_limit = 3

limits based on total integrated power at surface for all nuclear reactions

excluding photodistintegrations

L_nuc = nuclear reaction total energy release for all nuclear reactions (Lsun units)

delta_lgL_nuc_limit

delta_lgL_nuc_hard_limit

delta_lgL_nuc_at_high_T_limit

delta_lgL_nuc_at_high_T_hard_limit

delta_lgL_nuc_at_high_T_limit_lgT_min

max_lgT_for_lgL_nuc_limit

When L_nuc is dropping, multiply limits by lgL_nuc_drop_factor.

ignore changes in lgL_nuc if max logT > max_lgT_for_lgL_nuc_limit.

limit for magnitude of change in lgL_nuc retry if max delta is greater than delta_lgL_nuc_hard_limit, ignore changes in lgL_nuc if value is less than lgL_nuc_burn_min

if max logT is > delta_lgL_nuc_at_high_T_limit_lgT_min then

use delta_lgL_nuc_at_high_T_limit and delta_lgL_nuc_at_high_T_hard_limit

else

use delta_lgL_nuc_limit and delta_lgL_nuc_hard_limit

at extreme temperatures, can have numerical jitters in this as a result of almost cancelling large positive and negative contributions of forward and reverse rates such as photodisintegration and rebuilding of he4 so if doing advanced burning, may want to turn off lgL_nuc limits above some max logT and turn on lgL_power_photo limits at a somewhat smaller max logT.

delta_lgL_nuc_limit = -1
delta_lgL_nuc_hard_limit = -1

delta_lgL_nuc_at_high_T_limit = -1
delta_lgL_nuc_at_high_T_hard_limit = -1
delta_lgL_nuc_at_high_T_limit_lgT_min = 1d99

max_lgT_for_lgL_nuc_limit = 1d99
lgL_nuc_burn_min = 0.5d0
lgL_nuc_drop_factor = 10

limits based on total integrated power at surface for photodistintegrations

L_photo = nuclear reaction total energy release for all photodistintegrations (Lsun units) note that photodistintegrations consume energy so the total released is negative. photodisintegrations become large during late burning at high temperatures. values for lgL_photo are based on L_by_category(iphoto)

delta_lgL_power_photo_limit

delta_lgL_power_photo_hard_limit

min_lgT_for_lgL_power_photo_limit

lgL_power_photo_burn_min

lgL_power_photo_drop_factor

Limit for magnitude of change in lgL_photo. If max delta is greater than delta_lgL_power_photo_hard_limit, retry with smaller timestep. ignore delta_lgL_power_photo_limit when max logT < min_lgT_for_lgL_power_photo_limit. Ignore changes in lgL_photo if value is less than lgL_power_photo_burn_min. When L_photo is dropping, multiply limits by lgL_power_photo_drop_factor.

delta_lgL_power_photo_limit = -1
delta_lgL_power_photo_hard_limit = -1
min_lgT_for_lgL_power_photo_limit = 9d0
lgL_power_photo_burn_min = 10d0
lgL_power_photo_drop_factor = 10

limits based on changes at photosphere

delta_lgTeff_limit

delta_lgTeff_hard_limit

Limit for magnitude of max change in log10 temperature at photosphere.

delta_lgTeff_limit = 0.01d0
delta_lgTeff_hard_limit = -1

delta_lgL_limit_L_min

delta_lgL_limit

delta_lgL_hard_limit

Limit for magnitude of change in log10(L_surf/Lsun). Only apply this limit when L_surf >= delta_lgL_limit_L_min (in Lsun units).

delta_lgL_limit_L_min = -100
delta_lgL_limit = 0.1d0
delta_lgL_hard_limit = -1

dt_div_min_dr_div_cs_limit

dt_div_min_dr_div_cs_hard_limit

limit for dt compared to explicit solver timescale (negative means no limit)

min_dr_div_cs = min over all cells of dr/csound (seconds)

dt_div_min_dr_div_cs_limit = -1
dt_div_min_dr_div_cs_hard_limit = -1

dt_div_dt_cell_collapse_limit

dt_div_dt_cell_collapse_hard_limit

limit for dt compared to cell_collapse timescale (negative means no limit)

dt_cell_collapse = min over shells k that have v(k+1) > v(k) of
(r(k)-r(k+1))/(v(k+1)-v(k)), the time for the cell to collapse
to zero thickness at current velocities.  only for v_flag true.

dt_div_dt_cell_collapse_limit = -1
dt_div_dt_cell_collapse_hard_limit = -1

min_k_for_dt_div_min_dr_div_cs_limit

min_q_for_dt_div_min_dr_div_cs_limit

max_q_for_dt_div_min_dr_div_cs_limit

check_remnant_only_for_dt_div_min_dr_div_cs_limit

min_k_for_dt_div_min_dr_div_cs_limit = 20
min_q_for_dt_div_min_dr_div_cs_limit = 0.005d0
max_q_for_dt_div_min_dr_div_cs_limit = 0.995d0
check_remnant_only_for_dt_div_min_dr_div_cs_limit = .false.

min_abs_du_div_cs_for_dt_div_min_dr_div_cs_limit

min_abs_u_div_cs_for_dt_div_min_dr_div_cs_limit

only use dt_div_min_dr_div_cs_limit at cells where abs_du_div_cs > min_abs_du_div_cs_for_dt_div_min_dr_div_cs_limit and and abs_u_div_cs > min_abs_u_div_cs_for_dt_div_min_dr_div_cs_limit

allow focus on regions near shock face.

min_abs_u_div_cs_for_dt_div_min_dr_div_cs_limit = 0.8d0
min_abs_du_div_cs_for_dt_div_min_dr_div_cs_limit = 0.01d0

limits based on changes in location on HR diagram

delta_HR_ds_L

delta_HR_ds_Teff

dlgL = log10(L/L_prev)
dlgTeff = log10(Teff/Teff_prev)

delta_HR_ds_L = 1
delta_HR_ds_Teff = 1

delta_HR_limit

delta_HR_hard_limit

limit for dHR (negative means no limit)

dHR = sqrt((delta_HR_ds_L*dlgL)**2 + (delta_HR_ds_Teff*dlgTeff)**2)

delta_HR_limit = -1
delta_HR_hard_limit = -1

delta_lgT_max_limit

delta_lgT_max_hard_limit

delta_lgT_max_limit_lgT_min

delta_lgT_max_at_high_T_limit

delta_lgT_max_at_high_T_hard_limit

delta_lgT_max_at_high_T_limit_lgT_min

delta_lgT_max_limit_only_after_near_zams

limit for magnitude of change in max over all cells of log10 T this is for off center flashes in degenerate material (e.g., He or Ne) Only apply this limit when lgT_max >= delta_lgT_max_limit_lgT_min.

similarly, use at_high_T limits only when lgT_max >= delta_lgT_max_at_high_T_limit_lgT_min. this can be useful since higher order temperature sensitivity of rates at high T may require smaller limits for changes.

delta_lgT_max_limit = -1
delta_lgT_max_hard_limit = -1
delta_lgT_max_limit_lgT_min = 9d0

delta_lgT_max_at_high_T_limit = -1
delta_lgT_max_at_high_T_hard_limit = -1
delta_lgT_max_at_high_T_limit_lgT_min = -1

delta_lgT_max_limit_only_after_near_zams = .false.

limits based on changes at center

delta_lgT_cntr_limit

delta_lgT_cntr_hard_limit

delta_lgT_cntr_limit_only_after_near_zams

limit for magnitude of change in log10 temperature at center

delta_lgT_cntr_limit = 0.01d0
delta_lgT_cntr_hard_limit = -1
delta_lgT_cntr_limit_only_after_near_zams = .true.

delta_lgP_cntr_limit

delta_lgP_cntr_hard_limit

limit for magnitude of change in log10 pressure at center

delta_lgP_cntr_limit = -1
delta_lgP_cntr_hard_limit = -1

delta_lgRho_cntr_limit

delta_lgRho_cntr_hard_limit

limit for magnitude of change in log10 density at center

delta_lgRho_cntr_limit = 0.05d0
delta_lgRho_cntr_hard_limit = -1

dX_div_X_cntr is max(abs(xa(j,nz)-xa_old(j,nz))/xa(j,nz)) for any species j Small timesteps as the center carbon is exhausted.

delta_dX_div_X_cntr_min

Ignore changes in dX_div_X_cntr if value is less than this.

delta_dX_div_X_cntr_min = -5

delta_dX_div_X_cntr_max

Ignore changes in dX_div_X_cntr if value is more than this.

delta_dX_div_X_cntr_max = 0

delta_dX_div_X_cntr_limit

If max delta is greater than delta_dX_div_X_cntr_limit, reduce the next timestep by delta_dX_div_X_cntr_limit/max_delta.

delta_dX_div_X_cntr_limit = 0.1d0

delta_dX_div_X_cntr_hard_limit

If max delta is greater than delta_dX_div_X_cntr_hard_limit, retry with smaller timestep.

delta_dX_div_X_cntr_hard_limit = -1

lg_XH_cntr is log10(h1 mass fraction at center). Small timesteps as the center hydrogen is exhausted.

delta_lg_XH_cntr_min

Ignore changes in lg_XH_cntr if value is less than this.

delta_lg_XH_cntr_min = -6

delta_lg_XH_cntr_max

Ignore changes in lg_XH_cntr if value is more than this.

delta_lg_XH_cntr_max = 0

delta_lg_XH_cntr_limit

If max delta is greater than this, reduce the next timestep by delta_lg_XH_cntr_limit/max_delta.

delta_lg_XH_cntr_limit = 0.05d0

delta_lg_XH_cntr_hard_limit

If max delta is greater than delta_lg_XH_cntr_hard_limit, retry with smaller timestep.

delta_lg_XH_cntr_hard_limit = -1

lg_XHe_cntr is log10(he4 mass fraction at center) small timesteps as the center helium is exhausted.

delta_lg_XHe_cntr_min

Ignore changes in lg_XHe_cntr if value is less than this.

delta_lg_XHe_cntr_min = -6

delta_lg_XHe_cntr_max

Ignore changes in lg_XHe_cntr if value is more than this.

delta_lg_XHe_cntr_max = 0

delta_lg_XHe_cntr_limit

If max delta is greater than delta_lg_XHe_cntr_limit, reduce the next timestep by delta_lg_XHe_cntr_limit/max_delta.

delta_lg_XHe_cntr_limit = 0.1d0

delta_lg_XHe_cntr_hard_limit

If max delta is greater than delta_lg_XHe_cntr_hard_limit, retry with smaller timestep.

delta_lg_XHe_cntr_hard_limit = -1

lg_XC_cntr is log10(c12 mass fraction at center). Small timesteps as the center carbon is exhausted.

delta_lg_XC_cntr_min

Ignore changes in lg_XC_cntr if value is less than this.

delta_lg_XC_cntr_min = -5

delta_lg_XC_cntr_max

Ignore changes in lg_XC_cntr if value is more than this.

delta_lg_XC_cntr_max = 0

delta_lg_XC_cntr_limit

If max delta is greater than delta_lg_XC_cntr_limit, reduce the next timestep by delta_lg_XC_cntr_limit/max_delta.

delta_lg_XC_cntr_limit = 0.1d0

delta_lg_XC_cntr_hard_limit

If max delta is greater than delta_lg_XC_cntr_hard_limit, retry with smaller timestep.

delta_lg_XC_cntr_hard_limit = -1

lg_XO_cntr is log10(o16 mass fraction at center) Small timesteps as the center oxygen is exhausted.

delta_lg_XNe_cntr_min

Ignore changes in lg_XNe_cntr if value is less than this.

delta_lg_XNe_cntr_min = -5

delta_lg_XNe_cntr_max

Ignore changes in lg_XNe_cntr if value is more than this.

delta_lg_XNe_cntr_max = 0

delta_lg_XNe_cntr_limit

If max delta is greater than delta_lg_XNe_cntr_limit, reduce the next timestep by delta_lg_XNe_cntr_limit/max_delta.

delta_lg_XNe_cntr_limit = 1d99

delta_lg_XNe_cntr_hard_limit

If max delta is greater than delta_lg_XNe_cntr_hard_limit, retry with smaller timestep.

delta_lg_XNe_cntr_hard_limit = -1

delta_lg_XO_cntr_min

Ignore changes in lg_XO_cntr if value is less than this.

delta_lg_XO_cntr_min = -5

delta_lg_XO_cntr_max

Ignore changes in lg_XO_cntr if value is more than this.

delta_lg_XO_cntr_max = 0

delta_lg_XO_cntr_limit

If max delta is greater than delta_lg_XO_cntr_limit, reduce the next timestep by delta_lg_XO_cntr_limit/max_delta.

delta_lg_XO_cntr_limit = 1d99

delta_lg_XO_cntr_hard_limit

If max delta is greater than delta_lg_XO_cntr_hard_limit, retry with smaller timestep.

delta_lg_XO_cntr_hard_limit = -1

delta_lg_XSi_cntr_min

Ignore changes in lg_XSi_cntr if value is less than this.

delta_lg_XSi_cntr_min = -5

delta_lg_XSi_cntr_max

Ignore changes in lg_XSi_cntr if value is more than this.

delta_lg_XSi_cntr_max = 0

delta_lg_XSi_cntr_limit

If max delta is greater than delta_lg_XSi_cntr_limit, reduce the next timestep by delta_lg_XSi_cntr_limit/max_delta.

delta_lg_XSi_cntr_limit = 1d99

delta_lg_XSi_cntr_hard_limit

If max delta is greater than delta_lg_XSi_cntr_hard_limit, retry with smaller timestep.

delta_lg_XSi_cntr_hard_limit = -1

delta_XH_cntr_limit

If max delta is greater than this, reduce the next timestep by delta_XH_cntr_limit/max_delta.

delta_XH_cntr_limit = 0.01d0

delta_XH_cntr_hard_limit

If max delta is greater than delta_XH_cntr_hard_limit, retry with smaller timestep.

delta_XH_cntr_hard_limit = -1

delta_XHe_cntr_limit

If max delta is greater than delta_XHe_cntr_limit, reduce the next timestep by delta_XHe_cntr_limit/max_delta.

delta_XHe_cntr_limit = 0.01d0

delta_XHe_cntr_hard_limit

If max delta is greater than delta_XHe_cntr_hard_limit, retry with smaller timestep.

delta_XHe_cntr_hard_limit = -1

delta_XC_cntr_limit

If max delta is greater than delta_XC_cntr_limit, reduce the next timestep by delta_XC_cntr_limit/max_delta.

delta_XC_cntr_limit = 0.01d0

delta_XC_cntr_hard_limit

If max delta is greater than delta_XC_cntr_hard_limit, retry with smaller timestep.

delta_XC_cntr_hard_limit = -1

delta_XNe_cntr_limit

If max delta is greater than delta_XNe_cntr_limit, reduce the next timestep by delta_XNe_cntr_limit/max_delta.

delta_XNe_cntr_limit = 0.01d0

delta_XNe_cntr_hard_limit

If max delta is greater than delta_XNe_cntr_hard_limit, retry with smaller timestep.

delta_XNe_cntr_hard_limit = -1

delta_XO_cntr_limit

If max delta is greater than delta_XO_cntr_limit, reduce the next timestep by delta_XO_cntr_limit/max_delta.

delta_XO_cntr_limit = 0.01d0

delta_XO_cntr_hard_limit

If max delta is greater than delta_XO_cntr_hard_limit, retry with smaller timestep.

delta_XO_cntr_hard_limit = -1

delta_XSi_cntr_limit

If max delta is greater than delta_XSi_cntr_limit, reduce the next timestep by delta_XSi_cntr_limit/max_delta.

delta_XSi_cntr_limit = 0.01d0

delta_XSi_cntr_hard_limit

If max delta is greater than delta_XSi_cntr_hard_limit, retry with smaller timestep.

delta_XSi_cntr_hard_limit = -1

delta_dX_div_X_drop_only

delta_lg_XH_drop_only

delta_lg_XHe_drop_only

delta_lg_XC_drop_only

delta_lg_XNe_drop_only

delta_lg_XO_drop_only

delta_lg_XSi_drop_only

delta_XH_drop_only

delta_XHe_drop_only

delta_XC_drop_only

delta_XNe_drop_only

delta_XO_drop_only

delta_XSi_drop_only

If true, then only limit drops in abundance.

delta_dX_div_X_drop_only = .false.
delta_lg_XH_drop_only = .false.
delta_lg_XHe_drop_only = .false.
delta_lg_XC_drop_only = .false.
delta_lg_XNe_drop_only = .false.
delta_lg_XO_drop_only = .false.
delta_lg_XSi_drop_only = .false.
delta_XH_drop_only = .false.
delta_XHe_drop_only = .false.
delta_XC_drop_only = .false.
delta_XNe_drop_only = .false.
delta_XO_drop_only = .false.
delta_XSi_drop_only = .false.

limits based on changes in mass of the star

delta_lg_star_mass_limit

delta_lg_star_mass_hard_limit

Limit for magnitude of change in log10(M/Msun).

delta_lg_star_mass_limit = 5d-3
delta_lg_star_mass_hard_limit = -1

limit for change in mdot in Msun/yr + delta_mdot_atol tolerance for absolute changes + delta_mdot_rtol tolerance for relative changes

delta_mdot_atol = 1d-3
delta_mdot_rtol = 0.5d0

delta_mdot_limit

delta_mdot_hard_limit

delta_mot = abs(mdot - mdot_old)/ (delta_mdot_atol*Msun/secyer + &
   delta_mdot_rtol*max(abs(mdot),abs(mdot_old)))

ignore if < 0

delta_mdot_limit = -1
delta_mdot_hard_limit = -1

adjust_J_q_limit

adjust_J_q_hard_limit

limit for mass coordinate down to which angular momentum is adjusted when using do_adjust_J_lost

adjust_J_q_limit = 0.99
adjust_J_q_hard_limit = 0.98

limit_for_rel_error_in_energy_conservation

hard_limit_for_rel_error_in_energy_conservation

rel_error_in_energy_conservation = abs(error_in_energy_conservation/total_energy)

limit_for_rel_error_in_energy_conservation = 1d-4
hard_limit_for_rel_error_in_energy_conservation = 1d-3

report_min_dr_div_cs

If true, produce terminal output about minimum of cell dr/cs

report_min_dr_div_cs = .false.

report_dt_hard_limit_retries

If true, produce terminal output about choice of timestep.

report_dt_hard_limit_retries = .false.

report_solver_dt_info

If true, produce terminal output about choice of timestep based on varcontrol_target.

report_solver_dt_info = .false.

debugging controls

report_solver_progress

Set true to see info about solver iterations.

report_solver_progress = .false.

report_ierr

If true, produce terminal output when have some internal error.

report_ierr = .false.

report_bad_negative_xa

If true, produce terminal output when have bad negative mass fraction error.

report_bad_negative_xa = .false.

stop_for_bad_nums

If true, then stop for bad numbers (NaNs or infinity). this replaces old control stop_for_NaNs

stop_for_bad_nums = .false.

show_mesh_changes

When show_mesh_changes is true, the terminal output includes the mesh_call_number.

show_mesh_changes = .false.

trace_evolve

Send evolve output to screen.

trace_evolve = .false.

variety of output from the solver

solver_numerical_jacobian = .false.
solver_jacobian_nzlo = 1
solver_jacobian_nzhi = -1
solver_check_everything = .false.
solver_inspect_soln_flag = .false.
solver_test_partials_dx_0 = -1d0
solver_test_partials_k = -1
solver_test_partials_k_low = -1
solver_test_partials_k_high = -1
solver_test_eos_partials = .false.
solver_test_kap_partials = .false.
solver_test_net_partials = .false.
solver_test_atm_partials = .false.
solver_test_partials_var_name = ''
solver_test_partials_sink_name = ''
solver_test_partials_equ_name = ''
solver_test_partials_show_dx_var_name = ''
solver_show_correction_info = .false.
solver_test_partials_call_number = -1
solver_test_partials_iter_number = -1
solver_test_partials_write_eos_call_info = .false.
solver_epsder_struct = 1d-5
solver_epsder_chem = 1d-5

energy_conservation_dump_model_number = -1

solver_save_photo_call_number

Saves a photo when solver_call_number = solver_save_photo_call_number - 1

solver_save_photo_call_number = -1

xa_clip_limit

Abundances smaller than this limit are set to 0.

xa_clip_limit = 1d-99

fill_arrays_with_NaNs

initialize arrays with NaNs to trap reads of uninitialized entries.

fill_arrays_with_NaNs = .false.

zero_when_allocate

initialize arrays with zeros.

zero_when_allocate = .false.

miscellaneous controls

warn_rates_for_high_temp

If true then when any zone tries to evaluate a rate above max_safe_logT_for_rates it generates a warning message. The code will cap the rate at the value for max_safe_logT_for_rates whether the warning is on or not. 10d0 is a sensible default for the max temperature, as that is where the partition tables and polynomial fits to the rates are valid until. warning messages include the text “rates have been truncated” and “WARNING: evaluating rates”.

warn_rates_for_high_temp = .true.
max_safe_logT_for_rates = 10d0

warn_when_large_rel_run_E_err

message includes the text “WARNING: rel_run_E_err”

rel_run_E_err = abs(cumulative_energy_error/total_energy) you can turn off this warning message by setting this to a large number.

warn_when_large_rel_run_E_err = 0.1d0

absolute_cumulative_energy_err

cumulative energy error is the sum of the absolute value of per-step errors. Set this to .false. to allow positive and negative errors to cancel when integrating over multiple steps.

absolute_cumulative_energy_err = .true.

warn_when_stop_checking_residuals obsolete

warning_limit_for_max_residual

message includes the text “WARNING: max_residual > warning_limit_for_max_residual”

warning_limit_for_max_residual = 1d0

warn_when_large_virial_thm_rel_err

message includes the text “WARNING: virial_thm_rel_err” only applies to models with no velocities, rotation, or mass change.

warn_when_large_virial_thm_rel_err = 1d-2

warn_when_get_a_bad_eos_result

message includes the text “WARNING eos:”

warn_when_get_a_bad_eos_result = .true.

relax_dY

Change Y by this amount per step when relaxing Y.

relax_dY = 0.005d0

relax_dlnZ

Change lnZ by this amount per step when relaxing Z. Default is ln10/10.

relax_dlnZ = 2.3025850929940459d-1

eps_mdot_leak_frac_factor

eps_mdot_leak_frac_factor = 1d0

zams_filename

Default is for Z=0.02, Y=0.28.

zams_filename = 'zams_z2m2_y28.data'

set_rho_to_dm_div_dV = .true.

steps_before_start_stress_test

stress_test_relax

steps_before_start_stress_test = 0
stress_test_relax = .false.

use_other_{hook}

Logicals to deploy the use_other routines.

use_other_kap = .false.
use_other_diffusion = .false.
use_other_mlt_results = .false.

use_other_adjust_mdot = .false.
use_other_j_for_adjust_J_lost = .false.
use_other_alpha_mlt = .false.
use_other_am_mixing = .false.
use_other_brunt = .false.
use_other_brunt_smoothing = .false.
use_other_build_initial_model = .false.
use_other_cgrav = .false.
use_other_mesh_delta_coeff_factor = .false.

use_other_energy_implicit = .false.
use_other_energy = .false.
use_other_pressure = .false.
use_other_momentum_implicit = .false.
use_other_momentum = .false.
use_other_eps_grav = .false.
use_other_mesh_functions = .false.
use_other_D_mix = .false.
use_other_close_gaps = .false.

use_other_neu = .false.
use_other_net_get = .false.
use_other_solver_monitor = .false.
use_other_opacity_factor = .false.
use_other_diffusion_factor = .false.
use_other_diffusion_coefficients = .false.
use_other_pgstar_plots = .false.
use_other_gradr_factor = .false.
use_other_eval_fp_ft = .false.
use_other_torque = .false.
use_other_screening = .false.
use_other_rate_get = .false.
use_other_net_derivs = .false.
use_other_split_burn = .false.

use_other_torque_implicit = .false.
use_other_wind = .false.
use_other_after_struct_burn_mix = .false.
use_other_before_struct_burn_mix = .false.
use_other_surface_PT = .false.
use_other_remove_surface = .false.
use_other_set_pgstar_controls = .false.
use_other_accreting_state = .false.
use_other_eval_i_rot = .false.

use_other_export_pulse_data = .false.
use_other_get_pulse_data = .false.
use_other_edit_pulse_data = .false.

use_other_astero_freq_corr = .false.

use_other_timestep_limit = .false.

mixing diffusion coeffs

sig_term_limit

Limit on coefficients in convective mixing equations. Consider a diffusion eqn of form:

x(k) - x0(k) = c1*(x(k-1) - x(k)) - c2*(x(k) - x(k+1))

Simplify for c1=c2=c, x(k-1)=x(k+1)=x0(k)=x0, x(k)=x0+dx Then eqn becomes

(1+2*c)*(x0+dx) - 2*c*x0 = x0

If 2*c >> 1, then eqn becomes ill-conditioned, so we enforce c <= sig_term_limit In physical terms c is dt*sig/dm, where sig = (4 pi r^2 rho)^2*D and D = diffusion coeff (cm^2/s), so c can get large when dt/dm is large.

sig_term_limit = 1d13

am_sig_term_limit

Limit on coefficients in angular momentum transport equations. Necessary for numerical stability. Plays same role as sig_term_limit for material mixing.

am_sig_term_limit = 1d13

sig_min_factor_for_high_Tcenter

High center T limit to avoid negative mass fractions. If Tcenter >= Tcenter_min_for_sig_min_factor_full_on, then okay to reduce sig by as much as this factor as needed to prevent causing negative abundances. Inactive when >= 1d0.

sig_min_factor_for_high_Tcenter = 0.01d0

Tcenter_min_for_sig_min_factor_full_on

If Tcenter >= this, factor = sig_min_factor_for_neg_abundances, this should be > Tcenter_max_for_sig_min_factor_full_off.

Tcenter_min_for_sig_min_factor_full_on = 3.2d9

Tcenter_max_for_sig_min_factor_full_off

If Tcenter <= this, factor = 1, so has no effect this should be < Tcenter_min_for_sig_min_factor_full_on. For T > full_off and < full_on, factor changes linearly with Tcenter.

Tcenter_max_for_sig_min_factor_full_off = 2.8d9

max_delta_m_to_bdy_for_sig_min_factor

sig_min factor goes to 1 as distance (in Msun units) from boundary of mixing region reaches this value

max_delta_m_to_bdy_for_sig_min_factor = 0.5d0

delta_m_upper_for_sig_min_factor

okay to change sig min factor to 1 for mix region larger than this

delta_m_upper_for_sig_min_factor = 0.3d0

delta_m_lower_for_sig_min_factor

don’t change sig min factor for mix region smaller than this

delta_m_lower_for_sig_min_factor = 0.1d0

extra params as a convenience for developing new features note: the parameter num_x_ctrls is defined in star_def.inc

x_ctrl(1:num_x_ctrls) = 0d0
x_integer_ctrl(1:num_x_ctrls) = 0
x_logical_ctrl(1:num_x_ctrls) = .false.
x_character_ctrl(1:num_x_ctrls) = ''

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

read_extra_controls_inlist(1..5)

extra_controls_inlist_name(1..5)

If read_extra_controls_inlist(1) is true, then read &controls from this namelist file.

read_extra_controls_inlist(:) = .false.
extra_controls_inlist_name(:) = 'undefined'

save_controls_namelist

dumps all values for &controls namelist to file

save_controls_namelist = .false.

controls_namelist_name

if empty, uses a default name

controls_namelist_name = ''