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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.
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
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.
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
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.fxa_surface_lower_limit contains the lower limit value
upper limits on surface mass fractionsstop when surface abundance rises above this limitcan 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
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 atransistent velocity spike causing the model to prematurely exit. In solar masses
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 atransistent velocity spike causing the model to prematurely exit. In solar masses
Threshold for weighted smoothing of gradL_composition_term. Only apply smoothing (controlledby num_cells_for_smooth_gradL_composition_term) for contiguous regions where \(\nabla_L\) exceedsthis threshold. Might be useful for preventing narrow composition jumps from being excessivelybroadened by smoothing
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
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 transportSee gradT_excess_f1, gradT_excess_f2, and gradT_excess_age_fraction below.
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).
The switch from convective mixing to overshooting happens at a distance f0*Hp into the convection zonefrom the estimated location where grad_ad = grad_rad, where Hp is the pressure scale height at that location.A value
You can specify a range of star masses over which overshootingabove 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 instar_data/public/star_data_def.inc (currently 16)
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 smallconvective region at the core can produce excessively large overshooting because ofa large pressure scale height at the center.
Even if a region reaches the above temperature to be considered asa z_burn region, only set it as such if the helium mass fractionin 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 isconsidered as a he_burn region in terms of the hydrogen mass fraction.
Predictive mixing is controlled by specifying a set of parameters, which combines matchingcriteria (determining which boundaries to apply the predictive mixing to) together withvalues (determining how the predictive mixing should operate at those boundaries). Up toNUM_PREDICTIVE_PARAM_SETS of these parameter sets can be defined (see star_def.inc for value).
Matching criterion for the location of the convection zone. Possible values are core(the core convection zone), shell (a convective shell), surf (the surface convectionzone) or any (which matches any location).
Threshold for minimum superadiabaticity in the predictive mixing scheme; boundaryexpansion stops when gradr/grada-1 drops below this threshold. Default value is usuallygood for main-sequence evolution; for core He-burning, set to 0.005, 0.01 or largerto prevent splitting of the core convection zone and/or core breathing pulses.
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.
Parameters of the convection model.Note that RSP_alfap, RSP_alfas, RSP_alfac, RSP_alfad and RSP_gammarare expressed in the units of standard values.Standard values are the ones for which static version of the Kuhfussmodel reduces to standard MLT. See Table 1 in Smolec & Moskalik (2008)for standard values and the description of the parameters.
Initial kick makes use of the scaled linear velocity eigenvectorof a given mode or of the linear combination of the eigenvectorsfor the fundamental mode and first two radial overtones.The surface velocity is set to RSP_kick_vsurf_km_per_sec andthe mode content is set by RSP_fraction_1st_overtone and RSP_fraction_2nd_overtone
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 pulsationstate may depend on initial conditions set by the three parameters above.Integration of the same model with different initial kicks is a way to studythe nonlinear mode selection - for an example see Fig. 1 in Smolec & Moskalik (2010).
artificial viscosity controlsfor the equations see: Appendix C in Stellingwerf (1975).In principle, for not too-non-adiabatic convective models artificial viscosity is notneeded or should be very small. Hence a large cut-off parameter below (in purelyradiative models the default value for cut-off was 0.01)
zsh > 0 delays onset of artificial viscositycan 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
as described in section 4.2 of mesa3, 2015.RSP_Qvisc_linear is analogous to shock_spread_linearRSP_Qvisc_quadratic is analogous to shock_spread_quadraticif 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
Re-evaluate mixing info after each evolve step. This is helpful if you want the profiles toreflect the mixing params after the step; otherwise, they give the mixing info from the startof the step (i.e., one step out-of-date)
adjust angular momentumWith do_adjust_J_lost = .false., the angular momentum removed via windsfrom 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 avoidthis, the do_adjust_J_lost option adjusts the angular momentum contentof layers below those removed, such that
This can also be used to model mass loss mechanisms that remove moreangular momentum than mass_lost*s% j_rot_surf, for instance magneticbraking or wind mass loss. In that case, you can use theuse_other_j_for_adjust_J_lost option to specify a specific angular momentumof removed material different from j_rot_surf
if premix_omega is true, then do 1/2 of the transport of angular momentumbefore 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 whenusing do_adjust_J_lost.
if the relative change in total angular momentum exceeds these values,then a warning is given on the terminal output, or the simulation is stoppedaltogether. Not applied when using other_torque routines or for binaries.
Controls how the surface temperature Tsurf and pressure Psurf are evaluated whensetting up outer boundary conditions. We caution that the use of 'fixed_' atmosphereoptions might conflict with mlt_option = TDC.
'table':set Tsurf and Psurf by interpolating in pre-calculated tables based on modelatmospheres. 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 baseof 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 thetable BCs, and there is no particular location identified as the photosphere, sowe fall back to the surface values of L, R, and m to calculate quantities such asTeff and log_g. This is consistent with the assumptions used for table construction:geometrically thin atmospheres with constant flux.
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 ofthis boundary condition implemented via the other_surface_PT hook.
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