List of Parameters by Number
Number |
Name |
Format |
Default |
Unit |
Synopsis |
|---|---|---|---|---|---|
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Initial or current timestep. |
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Initial or current time. |
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Extrapolation Parameter used in guessing new |
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Quadratic artificial viscosity ( |
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Maximum number of times subroutine |
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Maximum desired fractional change in radius per step. |
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Maximum desired fractional change in temperature per step. |
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Maximum desired fractional change in density per step. |
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Maximum desired fractional linear contraction per step. |
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Maximum fractional change in the timestep per step. |
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Maximum allowed relative convergence error in radius. |
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Maximum allowed relative convergence error in temperature. |
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Linear artificial viscosity factor. |
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Maximum number of cycles. |
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Stop time. |
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Number of cycles between ASCII edits. |
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Time between ASCII edits ( |
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Number of cycles between restart dumps. |
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Ratio of the convective mixing length to the pressure scale height. |
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Fudge factor for convection (about |
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Multiplier for the rate of convective mixing. |
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Reduce timestep by dtcut (p 53) and redo step if convergence error in radius is still greater than fcrbu (p 22) after maxit (p 5) iterations. |
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Reduce timestep by dtcut (p 53) and redo step if convergence error in temperature is still greater than fctbu (p 23) after maxit (p 5) iterations. |
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Semi-convective mixing will be slower than thermal transport by
at least drmult (p 24) (about |
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Maximum timestep allowed. |
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Factor used to reduce noise in radius extrapolation. |
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Factor used to reduce noise in temperature extrapolation. |
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Abundance update parameter. Update abundances only if ipup (p 28)
:math:’ne’ |
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Multiplier on |
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Multiplier on |
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Multiplier on Christy opacity. |
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Multiplier on Compton opacity. |
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Multiplier on conductive opacity. |
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Ion energy and pressure multiplier. |
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Radiation energy and pressure multiplier. |
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Electron energy and pressure multiplier. |
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Multiplier on diffusive heat transport. |
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Time at which any |
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If iytsflag (p 67) |
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If iytsflag (p 67) |
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No further changes in |
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Size of graphics window to be created in the form |
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Multiplier on the inertial terms in the momentum balance equation. |
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Maximum length of a post-processor dump file. |
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Location of the top-left-hand corner of the graphics window relative
to top-left corner of screen, given in the form |
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Maximum desired fractional change in abundances per step. |
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Minimum elemental mass fraction that effects the timestep. |
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Velocity centring parameter (Range: |
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Opacity will be no larger than xkmin (p 50) + t7peek (p 49) |
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Least upper opacity bound. |
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Determine whether zones are considered in thermal equilibrium depending on time step and optical thickness. |
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Maximum number of times a given step is redone before the code quits. |
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Fractional timestep reduction when a step is redone. |
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If the maximum fractional change in radius during a
timestep exceeds tfcrbu (p 54) |
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If the maximum fractional change in temperature during a
timestep exceeds tfctbu (p 55) |
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Ionization potential. |
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Characteristic density for pressure ionization. |
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Pairs are included in EOS calculation only if npflag (p 58) |
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If the semi convective test parameter, |
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Radius of inner boundary. |
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Mass inside inner boundary. |
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Luminosity emerging from inner boundary. |
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Network switch parameter. |
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Graphics edits to the monitor are made every npixedit (p 64)
KEPLER cycles (if itvstart (p 127) |
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Don’t calculate nuclear burning in APPROX if the temperature is less than tnucmin (p 65). |
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Initialize new parameters in subroutine |
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Consider only specific changes in |
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Temperature at outer boundary. |
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Pressure at outer boundary. |
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Maximum allowed relative convergence error in luminosity. |
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Factor used to reduce noise in luminosity extrapolation. |
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Maximum desired fractional change in luminosity per step. |
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Reduce timestep by dtcut (p 53) and redo step if convergence error in luminosity is still greater than fclbu (p 73) after maxit (p 5) iterations. |
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If the maximum fractional change in luminosity during a
timestep exceeds tfclbu (p 74) |
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The fractional amount of semi convective mixing that can occur in one timestep is limited to approximately dtsmult (p 75). |
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Maximum fractional radius change allowed between zones before adzoning. |
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Minimum fractional radius change allowed between zones before dezoning. |
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Maximum fractional temperature change allowed between zones before adzoning. |
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Minimum fractional temperature change allowed between zones before dezoning. |
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Maximum fractional density change allowed between zones before adzoning. |
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Minimum fractional density change allowed between zones before dezoning. |
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Minimum radius for which adzoning is considered. |
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Minimum temperature for which adzoning is considered. |
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Minimum density for which adzoning is considered. |
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Minimum number of zones allowed after dezoning. |
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General rezoning flag. |
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Dezoning Flags. |
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Maximum radius for which rezoning is considered. |
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Minimum amount of potential hydrogen burn in the present timestep needed to trigger the use of any reaction network. |
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Minimum amount of |
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Mass fraction of heavy elements above which |
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Relative convergence required in calculating the electron Fermi
degeneracy parameter, |
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Innermost zone in which there is neutrino deposition. |
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Outermost zone in which there is neutrino deposition. |
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Total neutrino deposition energy. |
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Time of neutrino deposition. |
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Time scale for neutrino deposition. |
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Artificial neutrino core pressure parameter. |
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Core density cutoff. |
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Core pressure density dependence exponent. |
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Neutrino energy loss rate multiplier (APPROX only). |
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Non-neutrino nuclear energy generation rate multiplier (APPROX only). |
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|
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Fractional density and temperature perturbations used to get nuclear energy generation rate derivatives. |
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Increase the rezoner’s sensitivity to temperature gradients by a
factor of tcorefac (p 104) in the region where |
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Floor on the temperature used in the ISE calculation. |
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Change all APPROX network zones with |
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Multiply q1fac (p 13) by artv1 (p 107) in zone |
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Multiply q1fac (p 13) by artv2 (p 108) in zone |
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Multiply q1fac (p 13) by artv3 (p 109) in zone |
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See artv1 (p 107) - artv3 (p 109). |
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See artv1 (p 107) - artv3 (p 109). |
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See artv1 (p 107) - artv3 (p 109). |
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Graphics picture-type control parameter:. |
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Label each curve with nplotsym (p 114) character symbols. |
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Characteristic temperature for choosing the location of the temperature plotting grid in Thermodynamics (TD) graph. |
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Grid choice for the radial coordinate (irtype (p 132) |
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Obsolete. |
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Obsolete. |
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Innermost zone to plot. |
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Outermost zone to plot is |
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Minimum radius plotted when jp0 (p 119) |
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Maximum radius plotted when jp1 (p 120) |
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Lower bound of thermodynamics graph ordinate shall be no greater than ymintd (p 123). |
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Upper bound of thermodynamics graph ordinate shall be no less than ymaxtd (p 124). |
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Energy generation rate graph scale multiplier in the TD graph. |
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Pressure graph scale multiplier in the TD graph. |
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Graphics device control parameter. |
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Least elemental mass fraction plotted or listed in a terminal ion edit. |
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Obsolete. |
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Velocity graph scale multiplier in the TD graph. |
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Radius graph scale multiplier in the TD graph. |
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Ordinate value at which to plot convection sentinels in the TD graph. |
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Minimum fractional mass coordinate ( |
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Maximum fractional mass coordinate ( |
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Electron degeneracy parameter, |
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Enable Adaptive BURN network adjustment. |
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Multiplier in the effective values of the density, temperature, and radius gradients used to determine the necessity for adzoning or dezoning. |
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See fracrz1 (p 138) and fmax0 (p 150). |
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See fracrz1 (p 138). |
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See fracrz1 (p 138). |
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See fracrz1 (p 138). |
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Limiting ratio for |
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See abarrat0 (p 143). |
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See abarrat0 (p 143). |
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Don’t do convection if the absolute value of the zone velocity exceeds frcsound (p 146) times the local sound speed. |
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Limit the convective velocity to a fraction convlim (p 147) of the local sound speed. |
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The semiconvective test parameter, |
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The mass used in calculating ion degeneracy is xmimult (p 149) times the mass of a neutron. |
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Adzone mass fraction parameter. |
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See fmax0 (p 150). |
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See fmax0 (p 150). |
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Maximum fractional change in density since the last iteration
for which |
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Maximum fractional change in temperature since the last iteration for which ABAR changes and energy generation rates can be extrapolated from their previous values (APPROX only). |
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Extrapolate energy generation rates and |
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Save every nsdump (p 156) restart dumps. |
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Total number of cycles used to compute |
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Maximum allowed value of |
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Autumated ASCII and graphical output. |
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The mean atomic weight, |
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The effective number of zones used in |
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Effective number of zones used in subroutine |
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Don’t calculate derivatives in subroutine |
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Number of dump cycles between forced dumps of all dump-grid points of all ‘ions’ specified as dump variables. |
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Number of dump cycles between forced dumps of all dump-grid points of all BURN ‘isotopes’ specified as dump variables. |
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Number of dump cycles between forced dumps of all dump-grid points of all arrays specified as dump variables except ‘ions’ and ‘isotopes’. |
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The electron EOS is implicitly coupled to
nuclear burning-induced changes in the electron abundance,
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Make a ISE edit every njeditq (p 168) zones. |
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Relative temperature change used in calculating numerical
derivatives in |
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Relative density change used in calculating numerical
derivatives in |
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Include excited states in ISE calculations only if iexciteh (p 171)
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Maximum number of iterations allowed in ISE calculation. |
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Allowed relative convergence error in the proton abundance in the ISE calculation. |
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Allowed relative convergence error in the neutron abundance in the ISE calculation. |
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Allowed relative convergence error in the Si28 abundance in the ISE calculation. |
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Increment the proton, neutron, and |
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Maximum allowed relative change in proton abundance during an ISE iteration. |
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Maximum allo~ed relative change in neutron abundance during an ISE iteration. |
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Maximum allowed relative change in Si28 abundance during an ISE iteration. |
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Make a detailed edit of the ISE zones every neditq (p 180) general numerical edits. |
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If the relative change of the proton, neutron, or |
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See xiter1qe (p 181). |
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Edit only those ISE isotopes with mass fractions exceeding xthres (p 183). |
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A sufficient condition to change a zone from the APPROX to
ISE network is if its temperature exceeds tqselim (p 184),
its |
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See tqselim (p 184). |
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See tqselim (p 184). |
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Multiplier on neutrino energy losses from weak processes on nuclei and nucleons. |
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Change all ISE zones with |
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A sufficient condition to change a zone from the ISE to the NSE network is for the sum of the silicon and sulphur “group” elemental mass fractions to be less than or equal to siqselim (p 189). |
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Remove the inner jlcalc (p 190) zones from the problem and reset the inner boundary conditions on radius, radius0 (p 60), and mass, summ0 (p 61), but don’t change the central luminosity, xlum0 (p 62). |
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The ordinate bounds of the velocity graph are |
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Pause the code at the end of the calculation for zone
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See fracrz1 (p 138) and fmax0 (p 150). |
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See fracrz1 (p 138). |
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See fmax0 (p 150). |
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Multiplier on the contribution of ionization potential energy
to the equation of state. See subroutine |
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Start a new labelled ASCII output file every nnewoutf (p 197) cycles. |
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Make an ISE edit for the central zone every neditq1 (p 198)
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Multiplier on the Wilson-based nuclear EOS (except for thee thermal
ion component) if it is |
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Upper bound on the temperature used to calculate the energy in nuclear excited states and nuclear partition functions. |
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Initial guess made in |
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Neutron-rich-silicon-burning flows are included in the ISE
network if isi30brn (p 202) |
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Nominal minimum density for changing a zone from the APPROX to the ISE network. |
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Force a backup after a call to subroutine BURN from subroutine
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Maximim allowed fractional change in abundance before an abundance backup is made. (See abunminx (p 204)). |
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Elemental mass fraction floor for making abundance backups. (See abunminx (p 204)). |
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Fatal errors in |
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Multiplier on the overall |
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Limit how fast convective velocity can increase. |
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Flags regulating transition to QSE for convectively coupled zones. |
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Rate at which mass in the form of new zones is added to the surface of the star. |
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Mass of phantom outer zone used to mediate mass accretion. See accrate (p 211). |
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Allowed fractional convergence error in density when calculating a hydrostatic initial stellar configuration in the generator using the dstat option. |
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Characteristic flame radius for carbon deflagration studies. |
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Multiplier on the Wigner-Seitz Coulomb corrections to the ion
energy and pressure (See [Cla], p. 152, and subroutine |
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Rezoning Option Flag. |
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If nsurfz (p 217) |
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Inner surface zoning parameter. |
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Outer surface zoning parameter. |
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Multiplier on the de Jager mass-loss rate. |
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Nominal mass loss rate from the surface of the star. |
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The original total mass of the star. |
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Dezone the mass-losing zone if its mass drops below fracdez (p 223) times the average mass of the zones on either side of it. |
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Redo the timestep (“backup”) if the fractional change of mass in the mass-losing zone exceeds xmratbak (p 224). |
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Subtract any “surface” mass loss specified by xmlossm (p 220) or
xmloss0 (p 221) from the zone closest to the surface that still has
more than |
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Obsolete. |
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Multiplier on the E1 part of the |
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Multiplier on the E2 part of the |
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Do a forced update of BURN isotopic abundances in every zone every nupdate (p 229) cycles. |
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When BURN co-processing is initiated, or when the zerotime or reset commands are given, (re)set the zonal timesteps used by the BURN coprocessor to dtfrac (p 230) * dtnew (p 1). |
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BURN co-processing is skipped if a zone’s exterior mass coordinate is less than bmassmin (p 231). |
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BURN co-processing is skipped if a zone’s exterior mass coordinate is greater than bmassmax (p 232). |
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BURN co-processing is skipped if a zone’s temperature is less than btempmin (p 233). |
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BURN co-processing is skipped if a zone’s temperature is greater than btempmax (p 234). |
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BURN co-processing is skipped if the absolute value of a zone’s
normal nuclear energy generation rate ( |
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BURN co-processing is skipped if a zone’s density is less than bdenmin (p 236). |
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BURN co-processing is skipped if a zone’s density is greater than bdenmax (p 237). |
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Force a zone to be updated by the BURN coprocessor if its fractional temperature change since its last BURN processing exceeds tchange (p 238). |
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Force a zone to be updated by the BURN coprocessor if its fractional density change since its last BURN processing exceeds dchange (p 239). |
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BURN co-processing is skipped if a zone’s network number,
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Make a BURN isotopic abundance edit every neditb (p 241)
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Obsolete. |
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Make an elemental abundance edit every nedita (p 243) |
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Edit only zones whose zone number is |
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Make a BURN isotopic abundance edit for all zones every
neditall (p 245) |
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Minimum isotopic abundance that affects the calculation of the zonal timestep in the BURN coprocessor. |
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Maximum desired fractional change of an isotopic abundance used in determining the zonal timestep used in the BURN coprocessor. |
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Maximum factor by which the zonal timestep in the BURN coprocessor can be increased in one zonal cycle. |
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Back up to the previous zonal cycle in the BURN coprocessor if the new zonal timestep is less than dtbkup (p 249) times the previous timestep. |
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Make a complete ASCII edit of the nuclear processes in all zones considered by the BURN coprocessor every ncomp (p 250) cycles. |
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Make an ASCII edit of the nuclear processes in the central zone considered by the BURN coprocessor every ncent (p 251) cycles. |
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Make an ASCII edit of the nuclear processes involved every nedt (p 252) BURN coprocessor matrix inversions (debugging only). |
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Set newly calculated negative BURN isotope abundances to |
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|
Minimum absolute magnitude of a BURN matrix element for which Gauss-Jordan elimination is carried out in solving for changes in isotopic abundances. |
|
|
|
|
|
Total number of BURN-coprocessor matrix inversions so far (internally incremented). |
|
|
|
|
|
Total number of BURN-coprocessor backups so far (internally incremented). |
|
|
|
|
|
FORTRAN I/O unit number for |
|
|
|
|
|
Flag to switch on sparse matrix solver. |
|
|
|
|
|
Cumulative number of BURN coprocessor backups due to encountering negative isotopic abundances (incremented internally). |
|
|
|
|
|
Factor by which to reduce the BURN coprocessor zonal timestep when a negative isotopic abundance backup occurs. |
|
|
|
|
|
Minimum absolute magnitude ofa negative isotopic abundance (except of protons) that can cause a zonal backup in the BURN coprocessor. |
|
|
|
|
|
Minimum absolute magnitude of a negative proton abundance that can cause a zonal backup in the BURN coprocessor. |
|
|
|
|
|
Maximum number of consecutive negative isotopic abundance backups allowed in the BURN coprocessor before quitting. |
|
|
|
|
|
Number of coupled BURN co-processing / BURN isotope convection subcycles per KEPLER cycle. |
|
|
|
|
|
Use Fuller et. al.’s weak rates in the BURN coprocessor if
mazful (p 265) |
|
|
|
|
|
Decrease the abundance threshold for |
|
|
|
|
|
BURN coprocessing and related edits are done only if
inburn (p 267) |
|
|
|
|
|
Number of lines printed per “page” of ASCII output. |
|
|
|
|
|
Total number of non-BURN zonal arrays to save in restart dumps. |
|
|
|
|
|
Total number of BURN zonal arrays to save in restart dumps. |
|
|
|
|
|
Remove the outer zone if its velocity exceeds vloss (p 271) and its radius is larger than rlossmin (p 436), but do not change the previous values of pbound (p 69) and tbound (p 68). |
|
|
|
|
|
Edit only those BURN isotope mass-fractions whose values exceed abunlimb (p 272) in making terminal edits (including isotopic mass-fraction sums over zones). |
|
|
|
|
|
Mass unit used for the mass coordinate employed in making ASCII and terminal edits. |
|
|
|
|
|
Make an ascii edit of primary zonal quantities every
neditz1 (p 274) |
|
|
|
|
|
Make an ascii edit of secondary zonal quantities every
neditz2 (p 275) |
|
|
|
|
|
Flag determining the minimum amount of information printed in an ASCII cycle edit regardless of the settings of other edit parameters:. |
|
|
|
|
|
Effective value of medit (p 276) used in determining the scope of the final edit made when the problem is finished. |
|
|
|
|
|
Make an ascii edit of all changeable parameters every neditp (p 278)
|
|
|
|
|
|
Carbon mass fraction ahead of flame. |
|
|
|
|
|
Oxygen mass fraction for ne-ox problems. |
|
|
|
|
|
When the flame became RT unstable. |
|
|
|
|
|
Sharp1 parameter. |
|
|
|
|
|
Minimum speed from convection. |
|
|
|
|
|
Sharp2 parameter. |
|
|
|
|
|
(Edit only.). |
|
|
|
|
|
Time scale for the neutrino pulse considered by the BURN coprocessor in calculating neutrino-induced nucleosynthesis after core collapse. |
|
|
|
|
|
Total energy for the neutrino pulse considered by the BURN coprocessor in calculating neutrino- induced nucleosynthesis after core collapse. |
|
|
|
|
|
Temperature of the |
|
|
|
|
|
Temperature of the electron neutrinos in the neutrino pulse considered by the BURN coprocessor in calculating neutrino-induced nucleosynthesis after core collapse. |
|
|
|
|
|
Prevent separated islands of zones employing a new network from
developing by not letting zone |
|
|
|
|
|
Graphics character size for grid labels (relative to MONGO’s default character size). |
|
|
|
|
|
Graphics character size for curve labels (relative to MONGO’s default character size). |
|
|
|
|
|
Graphics character size for zone sentinels (relative to MONGO’s default character size). |
|
|
|
|
|
Graphics character size for header info (relative to MONGO’s default character size). |
|
|
|
|
|
Obsolete. |
|
|
|
|
|
Graphics window background color is white if ibackgnd (p 296)
|
|
|
|
|
|
Mass units used for the internal mass coordinate, |
|
|
|
|
|
Minimum number of points allowed in a dump grid. |
|
|
|
|
|
Number of KEPLER cycles between post-processor dump
cycles, i.e., calls to |
|
|
|
|
|
Length of the track(s) assigned to each dump variable in the post-processor dump(s). |
|
|
|
|
|
Maximum number of post-processor dump cycles beyond the
currently-specified dump cycle ( |
|
|
|
|
|
Default number of post-processor dump cycles between LOOK plots or prints or reconstructed TIMEMAP grids. |
|
|
|
|
|
If the fractional change in a dump variable since the last dump
cycle exceeds backfacq (p 303) |
|
|
|
|
|
Terminate the problem when the central temperature reaches TEMPSTOP. |
|
|
|
|
|
Terminate the problem when the central density reaches denstop (p 305). |
|
|
|
|
|
Terminate the problem when the infall velocity below vinstopm (p 462) exceeds vinstop (p 306). |
|
|
|
|
|
Terminate the problem when the |
|
|
|
|
|
Time at which to make the zero-age-main-sequence (ZAMS) parameter
changes and restart dump (typically |
|
|
|
|
|
Reset the value of izonef (p 86) to izonezms (p 309) at the time specified by timezms (p 308). |
|
|
|
|
|
Reset the value of q1fac (p 13) to q1faczms (p 310) at the time specified by timezms (p 308). |
|
|
|
|
|
Central temperature at which to make the pre-carbon-ignition
parameter changes and restart dump (typically |
|
|
|
|
|
Reset the value of yfloorx (p 47) to yflrxcig (p 312) when the central temperature specified by tempcig (p 311) is reached. |
|
|
|
|
|
Reset the value of fmaxm (p 195) to fmaxmcig (p 313) when the
central temperature specified by tempcig (p 311) is reached
if fmaxmcig (p 313) |
|
|
|
|
|
Reset the value of fmax0 (p 150) to fmax0cig (p 314) when the
central temperature specified by tempcig (p 311) is reached if
fmax0cig (p 314) |
|
|
|
|
|
Cumulative amount of time by which the problem time has been offset by zerotime commands. |
|
|
|
|
|
Lower mass-fraction limit of the isotopic abundance plot. |
|
|
|
|
|
Upper mass-fraction limit of the isotopic abundance plot. |
|
|
|
|
|
Number of BURN isotopes to be plotted, starting from the first one listed by the most recent setiso command. |
|
|
|
|
|
Reference time used in calculating the time coordinate in timeplots and timemaps. |
|
|
|
|
|
Reference offset time used in calculating the time-coordinate for timeplots and timemaps. |
|
|
|
|
|
Minimum value of the time-coordinate to be plotted in timeplots and timemaps (time coordinate units, see maptime (p 327)). |
|
|
|
|
|
Maximum value of the time-coordinate to be plotted in timeplots and timemaps (time coordinate units, see maptime (p 327)). |
|
|
|
|
|
Maximum value of |
|
|
|
|
|
Value of the zonal mean atomic weight, |
|
|
|
|
|
Semiconvective mixing will be slower than thermal transport by
at least drmultlo (p 325) (about |
|
|
|
|
|
The semiconvective test parameter, |
|
|
|
|
|
Flag indicating the desired time coordinate in timeplots and timemaps. |
|
|
|
|
|
Minimum value of the time map variable to be mapped. |
|
|
|
|
|
Maximum value of the timemap variable to be mapped. |
|
|
|
|
|
Minimum ratio of the minimum timemap variable limit to the maximum timemap variable limit in the case when the actual minimum value of the current timemap variable would otherwise be used as the minimum timemap limit. |
|
|
|
|
|
If the central temperature is |
|
|
|
|
|
If the central oxygen abundance is |
|
|
|
|
|
If the central temperature is |
|
|
|
|
|
If the central density is |
|
|
|
|
|
If the central mean atomic weight ( |
|
|
|
|
|
Minimum mass that a pair of zone may have and still be allowed to be adzoned. |
|
|
|
|
|
Calculate more accurate electron densities in partially ionized
regions if icalcne (p 337) |
|
|
|
|
|
Maximum allowable fractional convergence error in the electron
density calculated by subroutine |
|
|
|
|
|
Determine calculation of ionization. |
|
|
|
|
|
Minimum mass fraction for which an element is included in
the calculation of Saha ionization equilibrium done in
subroutine |
|
|
|
|
|
Assumed effective opacity for the deposition of gamma
ray energy from the radioactive decay of |
|
|
|
|
|
Dimensionless correction factor used in calculating the
escape of gamma rays from the radioactive decay of Ni56
and |
|
|
|
|
|
If the problem time is |
|
|
|
|
|
If the problem time is |
|
|
|
|
|
If the problem time is |
|
|
|
|
|
Default value of the first cycle to be read or plotted in making post-processor edits, time plots, or timemaps. |
|
|
|
|
|
Obsolete. |
|
|
|
|
|
The initial mass of the star being evolved (primary). |
|
|
|
|
|
The initial mass of the binary companion star. |
|
|
|
|
|
[PJH92]‘s alpha parameter, related to the angular momentum of the mass lost in binary transfer. |
|
|
|
|
|
[PJH92]‘s beta parameter. |
|
|
|
|
|
Initial binary separation. |
|
|
|
|
|
Mass loss rate due to binary mass transfer assumed when the primary stars exceeds its Roche radius. |
|
|
|
|
|
Current Roche radius. |
|
|
|
|
|
Langer mass loss rate parameter 1. |
|
|
|
|
|
Langer mass loss rate parameter 2. |
|
|
|
|
|
Initialization of ISE zones with |
|
|
|
|
|
Multiplier on GR corrections. |
|
|
|
|
|
Multiplier on gravitational constant. |
|
|
|
|
|
Energy deposition for GRB modelling. |
|
|
|
|
|
Obsolete. |
|
|
|
|
|
A parameter for Type Ia SNe simulations. |
|
|
|
|
|
Multiplier on Niewenhuijzen & de Jager mass loss rate. |
|
|
|
|
|
Enable rotationally-induced mixing. |
|
|
|
|
|
Molecular weight sensitivity of rotational mixing processes. |
|
|
|
|
|
Efficiency of chemical mixing by rotational instabilities. |
|
|
|
|
|
Efficiency of angular momentum transport by (semi)convection. |
|
|
|
|
|
Critical Reynolds number (affects secular shear instability). |
|
|
|
|
|
Critical Richardson number (do not change). |
|
|
|
|
|
General efficiency multiplier for dynamical shaer instability. |
|
|
|
|
|
General efficiency multiplier for Solberg-Hoiland instability. |
|
|
|
|
|
General efficiency multiplier for secular shear instability. |
|
|
|
|
|
General efficiency multiplier for Eddington-Sweet circulation. |
|
|
|
|
|
General efficiency multiplier for Goldreich-Schubert-Fricke instability. |
|
|
|
|
|
Under-relaxation factor on the corrections taken each iteration in the Henyey-solver. |
|
|
|
|
|
Write out convection plot file data ( |
|
|
|
|
|
Select opacity table. |
|
|
|
|
|
Multiplier on metallicity used in OPAL opacities. |
|
|
|
|
|
Metallicity-dependence of the mass loss. |
|
|
|
|
|
Secular rotational mixing processes may not change by more than that per time-step. |
|
|
|
|
|
Smooth some gradients used for computation of the rotational instabilities over that much grid points on either side. A Gaussian smoothing profile is used. |
|
|
|
|
|
Secular rotational mixing processes may change by at least that fraction for the local zonal diffusion time-scale. |
|
|
|
|
|
Secular rotational mixing processes may change by at least that fraction of the total diffusion coefficient. |
|
|
|
|
|
Paper dimensions in points (inch/72). |
|
|
|
|
|
Interior mass coordinate above which hydrostatic stratification is assumed. |
|
|
|
|
|
Surface mass coordinate above which hydrostatic stratification is assumed. |
|
|
|
|
|
Multiplier on WR mass loss rates. |
|
|
|
|
|
Set to value other than 0 to use old physics - mostly fix that energy generation in APPROX did not include neutrino losses and mass excess but only considered differences in binding energy. These are used as flags. |
|
|
|
|
|
Some SNIa stuff. |
|
|
|
|
|
Write out wind data to wind file |
|
|
|
|
|
Verbostiy of opacity subroutine. Zero gives no messages. |
|
|
|
|
|
Multiplier on limiting flux in radiation flux limiter. |
|
|
|
|
|
Limiting flux multiplied by. |
|
|
|
|
|
Limit to radiative flux of outer zone only if set to |
|
|
|
|
|
Write out total energies in file |
|
|
|
|
|
Minimum zone for production factor/yield plot. |
|
|
|
|
|
Maximum zone for production factor/yield plot. |
|
|
|
|
|
Take into account wind when computing production factors/yields. |
|
|
|
|
|
Determines the BURN abundance plot type (plot 9). |
|
|
|
|
|
Minimum mass number for production factor/yield plot;
automatic determination if set |
|
|
|
|
|
Maximum mass number for production factor/yield plot; automatic determination if set LE -99. |
|
|
|
|
|
Minimum value for yield in BURN plot types |
|
|
|
|
|
Maximum value for yield in BURN plot types |
|
|
|
|
|
Minimum value for density used in subroutine |
|
|
|
|
|
Central hydrogen abundance at which the #hdep dump is made. |
|
|
|
|
|
Central helium abundance at which the #hedep dump is made. |
|
|
|
|
|
Cycle frequency used to write *.enu data file. |
|
|
|
|
|
Minimum optical depth below (i.e., outside of) which zone are not allowed to become convective. |
|
|
|
|
|
Maximum radius beyond which zones are removed from star, similar to vloss (p 271). |
|
|
|
|
|
Minimum temperature below which zones are removed from star, similar to vloss (p 271) and rloss (p 409). |
|
|
|
|
|
Change zones back to APPROX network if temperature drops below tapprox (p 411). |
|
|
|
|
|
|
|
|
|
|
|
Minimum value for production factor in BURN plot types |
|
|
|
|
|
Maximum value for production factor in BURN plot types:n:0,
|
|
|
|
|
|
Minimum value for the mass fraction BURN plot types |
|
|
|
|
|
Maximum value for the mass fraction BURN plot types |
|
|
|
|
|
Minimum value of |
|
|
|
|
|
Record maximum abundances in BURN network (and save in the restart dumps if set to 1. |
|
|
|
|
|
Mass coordinate below which no BURN co-processing is considered. |
|
|
|
|
|
Central |
|
|
|
|
|
Version of the special rate set to use. |
|
|
|
|
|
Version of the APPROX network rate subroutine to use. |
|
|
|
|
|
Switch to enable magnetic fields according to [Spr02]. |
|
|
|
|
|
Convective zones are bound by overshooting layer only of they are at least nosht (p 424) zones thick. |
|
|
|
|
|
Efficiency factor for thermohaline convection. |
|
|
|
|
|
No rezoning is performed when the region under consideration contains
a step in |
|
|
|
|
|
No rezoning is performed when the region under consideration contains
a step in |
|
|
|
|
|
No rezoning is performed when the region under consideration
contains a step in the mean molecular weight,
|
|
|
|
|
|
Minimum APPROX network number until which BURN coprocessing is followed. |
|
|
|
|
|
|
|
|
|
|
|
Make the outermost ymcorot (p 431) rotate with angular velocity
|
|
|
|
|
|
Write out structure data file |
|
|
|
|
|
Determine when during cycle “”mixing” is being done. |
|
|
|
|
|
Substitute BURN network for APPROX network (including energy
generation, |
|
|
|
|
|
This parameter regulates the behaviour of lburn (p 434). |
|
|
|
|
|
Minimum radius for which to apply vloss (p 271). |
|
|
|
|
|
Number of outer layers to be written in light curve output file, .lc. |
|
|
|
|
|
Multiply |
|
|
|
|
|
Multiply |
|
|
|
|
|
Multiply eddy viscosity by considered in magnetic field model this factor. |
|
|
|
|
|
Multiply eddy diffusivity in magnetic field model by this factor. |
|
|
|
|
|
Backup if abundance change vector |
|
|
|
|
|
Control isotope/network used in abundance plots, Plot |
|
|
|
|
|
Do not rezone the innermost minzone (p 444) zones. |
|
|
|
|
|
Do not dezone zones bigger than zonemmax (p 445). |
|
|
|
|
|
Electron anti-neutrino temperature for core collapse neutrino flux. |
|
|
|
|
|
Number of levels per dex for .cnv output file. |
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
Minimum density for dezoning. |
|
|
|
|
|
Flag to switch off adzoning. |
|
|
|
|
|
Multiplier on dynamic time-scale used to determine whether to treat
problem (zones) as “dynamic” or “static” in subroutine
|
|
|
|
|
|
Hydrogen mass fraction at which to make the #hburn dump. |
|
|
|
|
|
Carbon mass fraction at which to make the #heign dump. |
|
|
|
|
|
Helium mass fraction at which to make the #heburn dump. |
|
|
|
|
|
Do not adzone a pair of zones with thickness below zonermin (p 457). |
|
|
|
|
|
Do not dezone zones with thickness greater than zonermax (p 458). |
|
|
|
|
|
Extent (in mass) of a linear composition gradient between substrate and newly accreted material. |
|
|
|
|
|
Determine accretion mass. |
|
|
|
|
|
The mass of newly accreted zone is may not differ by more than a factor (or fraction) accmassf (p 461) from the current outermost zone. |
|
|
|
|
|
||
|
|
|
|
Minimum mass number for which weak rates are modified. |
|
|
|
|
|
Multiplier on positron decay/electron capture rate for lowamul (p 463)
|
|
|
|
|
|
Multiplier on electron decay rate for lowamul (p 463) |
|
|
|
|
|
Maximum mass number for which weak rates are modified. |
|
|
|
|
|
Use of BURN abundances for opacity. |
|
|
|
|
|
Multiply opacity and its derivatives by fackap (p 468). |
|
|
|
|
|
Remove all outer shells that have an angular velocity
|
|
|
|
|
|
Use Langer’s (1998) formula for rotationally enhanced mass loss. |
|
|
|
|
|
Reduce angular momentum to Keplerian angular momentum in the surface layes down to an exterior mass of ymjkep (p 471) if it exceeds Keplerian rotation. |
|
|
|
|
|
Do not rezone outermost maxzone (p 472) zones. |
|
|
|
|
|
Metallicity dependent mass loss scaling with C abundance for cool Pop III stars. |
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
||
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
Minimum temperature for weak rates. |
|
|
|
|
|
Multiplier on simplistic centrifugal force. |
|
|
|
|
|
Write out mixing file |
|
|
|
|
|
Determine use of RPROX network. |
|
|
|
|
|
Version of N14(p,g) rate to use. |
|
|
|
|
|
Multiplier on triple-alpha reaction rate. |
|
|
|
|
|
Set BURN date warning messages. |
|
|
|
|
|
Activate fallback treatment. |
|
|
|
|
|
Neutrino magnetic moment in units of |
|
|
|
|
|
Number of older z files to save. |
|
|
|
|
|
Axion mass
|
|
|
|
|
|
Maximum mass for convection. |
|
|
|
|
|
Maximum radius for convection. |
|
|
|
|
|
Truncate binary output files on restart/generation. |
|
|
|
|
|
Recent version> Version of the current convection output file. |
|
|
|
|
|
Recent version> Version of the current wind output file. |
|
|
|
|
|
Mass fraction of |
|
|
|
|
|
WIMP mass. |
|
|
|
|
|
Minimum time between plot outputs in seconds. |
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
Spin-independent cross section of WIMPs on protons. |
|
|
|
|
|
Spin-independent cross section of WIMPs on protons. |
|
|
|
|
|
Spin-dependent cross section of WIMPs on protons. |
|
|
|
|
|
Spin-dependent cross section of WIMPs on protons. |
|
|
|
|
|
WIMP density. |
|
|
|
|
|
WIMP velocity dispersion. |
|
|
|
|
|
Velocity of star relative to WIMP dark matter halo. |
|
|
|
|
|
Network to use for WIMP cross section calculations. |
|
|
|
|
|
|
|
|
|
|
|
Mass coordinate (not including summ0 (p 61)) for which inner angular velocities angw0x (p 579), angw0y (p 580), and angw0z (p 510) are set. |
|
|
|
|
|
|
|
|
|
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Do not dezone zones with |
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Depth where mass is to be accreted. |
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Initial pulsar rotational energy. |
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Asymptotic pulsar magnetic field at late times. |
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Number of zones over which to distribute pulsar energy. |
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Maximum ratio of mass accreting zone before it is forced to
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Include energy term from advection in mass loss. |
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Include energy term from advection in accretion. |
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Advection of composition during accretion. |
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Minimum temperature for neutrino losses if APPROX and BURN are not active. |
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Choose atmosphere model for added boundary pressure
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Output log file if set to |
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Do nuclear burning/energy generation. |
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Do neutrino losses. |
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Minimum mass coordinate for APPROX network. |
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Minimum mass for neutrino losses. |
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Mode for “decretion” model. |
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Rate of mass decretion from inner zone. |
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Fraction of mass of inner zone for dezoning if in decretion mode. |
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Zone from which to remove mass in decretion. |
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Use |
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Multiply accretion time and time scale by this factor for accretion data from a file. |
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Multiply base luminosity time and time scale by this factor for accretion data from a file. |
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Write out data file for NuGrid every nsekout (p 536) cycles. |
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Verbosity of |
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Verbosity of |
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Switch on charged current neutrino reactions on |
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Switch on neutral current due to electron neutrinos if set to |
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Switch on neutral current due to electron anti-neutrinos if set to
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Overwriting of hard-coded and |
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Mass fraction of |
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Mass fraction of |
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Mass fraction of |
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Frequency to write out *.ent file. |
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Number of levels to write out in *.ent file. |
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Mass of level interval to write out into *.ent file. |
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Multiplier on luminosity from base from time-dependent input file. |
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Multiplier on accretion rate from time-dependent input file. |
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Rotational energy source from dissipation. |
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Strength of equipartition radial magnetic field used for simple
dynamo with magnet (p 423) |
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Strength of equipartition toroidal magnetic field used for simple
dynamo with magnet (p 423) |
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Density of newly accreted zone relative to outermost zone. |
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Time scale on which co-rotation is established. |
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Select BR for |
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Switch for |
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Write out data file for neutrino information every nnuout (p 558) cycles. |
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Initial magnetic field strength. |
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Decay time of initial magnetic field toward. |
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Rate of energy deposition from extra heating. |
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Center of mass where energy is deposited; mass is measured relative to surface. |
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Width ( |
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Maximum radius for which energy deposition for advection from accretion is considered. |
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Mass loss for super-eddignton luminosity. |
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Determine zone where values for Eddington luminosity mass loss are taken. |
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Flag to switch on local criterion for new mass grid on adzoning and dezoning. |
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Unit in which to measure accretion depth. |
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Don’t do convcetion outside convmass (p 569). |
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Use optical depth-based zoning where |
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Optical depth ratio used in rezoning. |
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Optical depth limit used in rezoning. |
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Multiplier on centrifugal force used for atmosphere boundary pressure. |
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Multiplier atmosphere boundary pressure. |
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Switch on 3D angular momentum. |
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Write out rotation data file. |
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Minimum density for weak rates. |
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General efficiency multiplier for generalised dynamical instability. |
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Relative weighing of Solberg-Hoiland instability contribution for generalised dynamical instability (angfjdyn (p 585)). |
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When set to |
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Multiplier on Rossby reference rotation profile. |
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Maximum value of gradient in Rossby reference rotation profile. |
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Power of Rossby number (Ro) in gradient of Rossby reference rotation profile. |
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Binary interaction type. |
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Maximum allowed relative change in mass loss rate. |
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Multiplier for convectively bound flame for O burning flame. |
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If set to |
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Fraction of neutrino energy in electron neutrinos. |
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Fraction of neutrino energy in electron anti-neutrinos. |
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Record and plot NSE/QSE isotope abundances. |
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Switch on CNET. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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For future CNET use. |
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First zone multiplier on change in radius per step. |
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First zone multiplier on change in temp per step. |
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First zone multiplier on change in lumin per step. |
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First zone multiplier on change in density per step. |
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First zone multiplier on linear contraction per step. |
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WR mass loss rate formula to use. |
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Mass loss bass for limiting relative change in mass loss rates. |
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Temperature of inner boundary. |
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Grid generation convergence limit. |
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Minimum opacity used for atmosphere model. |
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Maximum opacity used for atmosphere model. |
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Efficiency factor for convective entrainment. |
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Exponent for convective entrainment. |
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Write out interface data to file |
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Write out interface data for radius rifcout (p 626). Off when
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Recent version> Version of the current interface output file. |
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Flags for run termination. |
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Minimum time step for run. |
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Write out slight curve data file |
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Recent version> Version of the current lightcurve output file. |
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Free memory of old variable storage after convergence. May make code use slightly less memory at the expense of overhead for re-allocation of memory at the next cycle. |
,
,
and
values.
) factor.
).
, is
and then to
.
*
.
0.
, is
current version.
.
-axix type for plots.
, above which to use
temperature interpolation in subroutine
, provided
abundances by a
fraction
and
neutrinos in the
neutrino pulse considered by the BURN coprocessor in calculating
neutrino- induced nucleosynthesis after core collapse.
, is below
and
.
efficiency parameter for semiconvection according to
of more than
of more than
-component of co-rotation angular velocity.
. Off
if
) when
set to
.

) of the Gaussian in mass where energy is deposited.
-component of specific angular momentum of newly accreted material.