[mesa-users] Core mass and core radius

[Bill Paxton]

On Apr 22, 2013, at 12:26 PM, Richard Townsend wrote:

> Is there a straightforward way to have MESA write the He core mass and core radius to history.data during RGB evolution?


from star/defaults/history_columns.list

   ! information about abundance transitions
   
      h1_boundary_mass
         ! h1 boundary is first location going inward from surface
         ! with h1 abundance <= h1_boundary_limit
      h1_boundary_radius
      h1_boundary_lgT
      h1_boundary_lgRho
      !h1_boundary_L
      !h1_boundary_v
      !h1_bdy_to_phot_sound_time ! (seconds)
         ! time for sound wave to reach photosphere from h1 boundary
      
      !h1_bdy_omega
      !h1_bdy_omega_div_omega_crit

      he4_boundary_mass
         ! he4 boundary is first location going inward from h1 boundary
         ! with he4 abundance <= he4_boundary_limit
      he4_boundary_radius
      he4_boundary_lgT
      he4_boundary_lgRho
      !he4_boundary_L
      !he4_boundary_v
      !he4_bdy_to_phot_sound_time ! (seconds)
         ! time for sound wave to reach photosphere from he4 boundary
      !he4_bdy_omega
      !he4_bdy_omega_div_omega_crit

      !c12_boundary_mass
         ! c12 boundary is first location going inward from he4 boundary
         ! with c12 abundance <= c12_boundary_limit
      !c12_boundary_radius
      !c12_boundary_lgT
      !c12_boundary_lgRho
      !c12_boundary_L
      !c12_boundary_v
      !c12_bdy_to_phot_sound_time ! (seconds) 
         ! time for sound wave to reach photosphere from c12 boundary
      !c12_bdy_omega
      !c12_bdy_omega_div_omega_crit

      !iron_core_boundary_mass
         ! iron_core boundary is first location going inward from c12 boundary
         ! with Fe,Co,Ne... abundance <= iron_core_boundary_limit
      !iron_core_boundary_radius
      !iron_core_boundary_lgT
      !iron_core_boundary_lgRho
      !iron_core_boundary_L
      !iron_core_boundary_v
      !iron_core_bdy_to_phot_sound_time ! (seconds) 
         ! time for sound wave to reach photosphere from iron_core boundary
      !iron_core_bdy_omega
      !iron_core_bdy_omega_div_omega_crit

      !envelope_mass ! = star_mass - h1_boundary_mass
      !envelope_fraction_left ! = envelope_mass / (initial_mass - h1_boundary_mass)

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