! history_columns.list -- determines the contents of star history logs
! you can use a non-standard version by setting log_columns_file in your inlist

! units are cgs unless otherwise noted.

! reorder the following names as desired to reorder columns.
! comment out the name to omit a column (fewer columns => less IO => faster running).
! remove '!' to restore a column.

! if you have a situation where you want a non-standard set of columns,
! make a copy of this file, edit as desired, and give the new filename in your inlist
! as log_columns_file.   if you are just adding columns, you can 'include' this file,
! and just list the additions in your file.   note: to include the standard default
! version, use include '' -- the 0 length string means include the default file.

! blank lines and comments can be used freely.
! if a column name appears more than once in the list, only the first occurrence is used.

! if you need to have something added to the list of options, let me know....


! the first few lines of the log file contain a few items:

   ! version_number -- for the version of mesa being used
   ! burn_min1 -- 1st limit for reported burning, in erg/g/s
   ! burn_min2 -- 2nd limit for reported burning, in erg/g/s


! note: you can include another list by doing
!        include 'filename'
!        include '' means include the default standard list file


! the following lines of the log file contain info about 1 model per row

   ! some general info about the model

      model_number ! counting from the start of the run
      star_age ! elapsed simulated time in years since the start of the run
      !log_star_age
      star_mass ! in Msun units

      !star_gravitational_mass ! star_mass is baryonic mass
      !star_mass_grav_div_mass

      !delta_mass ! star_mass - initial_mass in Msun units
      !log_xmstar ! log10 mass exterior to M_center (grams)
      !star_mdot ! d(star_mass)/dt (in msolar per year)
      log_abs_mdot ! log10(abs(star_mdot)) (in msolar per year)
      !time_step ! timestep in years since previous model
      log_dt ! log10 time_step
      num_zones ! number of zones in the model
      !species ! size of net
      !log_total_angular_momentum


   ! mixing regions

      !mass_conv_core ! (Msun) mass coord of top of convective core.  0 if core is not convective


      !  mx1 refers to the largest (by mass) convective region.
      !  mx2 is the 2nd largest.

      !  conv_mx1_top and conv_mx1_bot are the region where mixing_type == convective_mixing.
      !  mx1_top and mx1_bot are the extent of all kinds of mixing, convective and other.

      ! values are m/Mstar
      !conv_mx1_top
      !conv_mx1_bot
      !conv_mx2_top
      !conv_mx2_bot
      !mx1_top
      !mx1_bot
      !mx2_top
      !mx2_bot

      ! radius -- values are radii in Rsun units
      !conv_mx1_top_r
      !conv_mx1_bot_r
      !conv_mx2_top_r
      !conv_mx2_bot_r
      !mx1_top_r
      !mx1_bot_r
      !mx2_top_r
      !mx2_bot_r

      ! you might want to get a more complete list of mixing regions by using the following

      !mixing_regions <integer> ! note: this includes regions where the mixing type is no_mixing.

        ! the <integer> is the number of regions to report
        ! there will be 2*<integer> columns for this in the log file, 2 for each region.
        ! the first column for a region gives the mixing type as defined in mlt/public/mlt_def.

        ! the second column for a region gives the m/mstar location of the top of the region
        ! entries for extra columns after the last region in the star will have an invalid mixing_type value of -1.
        ! mstar is the total mass of the star, so these locations range from 0 to 1
        ! all regions are include starting from the center, so the bottom of one region
        ! is the top of the previous one.  since we start at the center, the bottom of the 1st region is 0.

        ! the columns in the log file will have names like 'mix_type_1' and 'mix_qtop_1'

        ! if the star has too many regions to report them all,
        ! the smallest regions will be merged with neighbors for reporting purposes only.


      !mix_relr_regions <integer>
        ! same as above, but locations given as r/rstar instead of m/mstar.
        ! the columns in the log file will have names like 'mix_relr_type_1' and 'mix_relr_top_1'

    ! regions of strong nuclear burning

        ! 2 zones where eps_nuc > burn_min1 erg/g/s
        ! for each zone have 4 numbers: start1, start2, end2, end1
        ! start1 is mass of inner edge where first goes > burn_min1 (or -20 if none such)
        ! start2 is mass of inner edge where first zone reaches burn_min2 erg/g/sec (or -20 if none such)
        ! end2 is mass of outer edge where first zone drops back below burn_min2 erg/g/s
        ! end1 is mass of outer edge where first zone ends (i.e. eps_nuc < burn_min1)
        ! similar for the second zone

        !epsnuc_M_1 ! start1 for 1st zone
        !epsnuc_M_2 ! start2
        !epsnuc_M_3 ! end2
        !epsnuc_M_4 ! end1

        !epsnuc_M_5 ! start1 for 2nd zone
        !epsnuc_M_6 ! start2
        !epsnuc_M_7 ! end2
        !epsnuc_M_8 ! end1


        ! you might want to get a more complete list of burning regions by using the following

        !burning_regions <integer>
          ! the <integer> is the number of regions to report
          ! there will be 2*<integer> columns for this in the log file, 2 for each region.
          ! the first column for a region gives int(sign(val)*log10(max(1,abs(val))))
          ! where val = ergs/gm/sec nuclear energy minus all neutrino losses.
          ! the second column for a region gives the q location of the top of the region
          ! entries for extra columns after the last region in the star will have a value of -9999
          ! all regions are included starting from the center, so the bottom of one region
          ! is the top of the previous one.
          ! since we start at the center, the bottom of the 1st region is q=0 and top of last is q=1.

          ! the columns in the log file will have names like 'burn_type_1' and 'burn_qtop_1'


          ! if the star has too many regions to report them all,
          ! the smallest regions will be merged with neighbors for reporting purposes only.




      ! conditions at base of largest convection zone (by mass)
          !cz_bot_mass ! mass coordinate of base (Msun)
          !cz_mass ! mass coordinate of base (Msun) -- same as cz_bot_mass
          !cz_log_xmass ! mass exterior to base (g)
          !cz_log_xmsun ! mass exterior to base (Msun)
          !cz_xm ! mass exterior to base (Msun)
          !cz_logT
          !cz_logRho
          !cz_logP
          !cz_bot_radius ! Rsun
          !cz_log_column_depth
          !cz_log_radial_depth
          !cz_luminosity ! Lsun
          !cz_opacity
          !cz_log_tau
          !cz_eta
          !cz_log_eps_nuc ! log10(ergs/g/s)
          !cz_t_heat ! Cp*T/eps_nuc (seconds)

          !cz_csound
          !cz_scale_height
          !cz_grav

          !cz_omega
          !cz_omega_div_omega_crit

          !cz_zone

      ! mass fractions at base of largest convection zone (by mass)
          !cz_log_xa h1
          !cz_log_xa he4




      ! conditions at top of largest convection zone (by mass)
          !cz_top_mass ! mass coordinate of top (Msun)
          !cz_top_log_xmass ! mass exterior to top (g)
          !cz_top_log_xmsun ! mass exterior to top (Msun)
          !cz_top_xm ! mass exterior to top (Msun)
          !cz_top_logT
          !cz_top_logRho
          !cz_top_logP
          !cz_top_radius ! Rsun
          !cz_top_log_column_depth
          !cz_top_log_radial_depth
          !cz_top_luminosity ! Lsun
          !cz_top_opacity
          !cz_top_log_tau
          !cz_top_eta
          !cz_top_log_eps_nuc ! log10(ergs/g/s)
          !cz_top_t_heat ! Cp*T/eps_nuc (seconds)

          !cz_top_csound
          !cz_top_scale_height
          !cz_top_grav

          !cz_top_omega
          !cz_top_omega_div_omega_crit

          !cz_top_zone
          !cz_top_zone_logdq

      ! mass fractions at top of largest convection zone (by mass)
          !cz_top_log_xa h1
          !cz_top_log_xa he4

      ! information about cores

          he_core_mass
          !he_core_radius
          !he_core_lgT
          !he_core_lgRho
          !he_core_L
          !he_core_v
          !he_core_omega
          !he_core_omega_div_omega_crit

          c_core_mass
          !c_core_radius
          !c_core_lgT
          !c_core_lgRho
          !c_core_L
          !c_core_v
          !c_core_omega
          !c_core_omega_div_omega_crit

          o_core_mass
          !o_core_radius
          !o_core_lgT
          !o_core_lgRho
          !o_core_L
          !o_core_v
          !o_core_omega
          !o_core_omega_div_omega_crit

          si_core_mass
          !si_core_radius
          !si_core_lgT
          !si_core_lgRho
          !si_core_L
          !si_core_v
          !si_core_omega
          !si_core_omega_div_omega_crit

          fe_core_mass
          !fe_core_radius
          !fe_core_lgT
          !fe_core_lgRho
          !fe_core_L
          !fe_core_v
          !fe_core_omega
          !fe_core_omega_div_omega_crit

          neutron_rich_core_mass
          !neutron_rich_core_radius
          !neutron_rich_core_lgT
          !neutron_rich_core_lgRho
          !neutron_rich_core_L
          !neutron_rich_core_v
          !neutron_rich_core_omega
          !neutron_rich_core_omega_div_omega_crit

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

          !h_rich_layer_mass ! = star_mass - he_core_mass
          !he_rich_layer_mass ! = he_core_mass - c_core_mass
          !c_rich_layer_mass ! = c_core_mass - o_core_mass
          !o_rich_layer_mass ! = o_core_mass - si_core_mass
          !si_rich_layer_mass ! = si_core_mass - fe_core_mass



      ! info about locations where optical depth is 10 or 100

          !tau10_mass ! mass in solar units where optical depth = 10
          !tau10_radius ! radius in solar units where optical depth = 10
          !tau10_lgP ! estimate for log10(P) at tau = 10
          !tau10_T ! estimate for T at tau = 10
          !tau10_lgT ! estimate for log10(T) at tau = 10
          !tau10_lgRho ! estimate for log10(density) at tau = 10
          !tau10_L ! estimate for L/Lsun at tau = 10

          !tau100_mass ! location in solar units where optical depth = 100
          !tau100_radius ! location in solar units where optical depth = 100
          !tau100_lgP ! estimates for values at tau = 100
          !tau100_T
          !tau100_lgT
          !tau100_lgRho
          !tau100_L

      ! timescales

          dynamic_timescale ! dynamic timescale (seconds) -- estimated by 2*pi*sqrt(r^3/(G*m))
          kh_timescale ! kelvin-helmholtz timescale (years)
          mdot_timescale ! star_mass/abs(star_mdot) (years)
          !kh_div_mdot_timescales ! kh_timescale/mdot_timescale
          nuc_timescale ! nuclear timescale (years) -- proportional to mass divided by luminosity
          !log_chem_timescale ! burn+mix timescale (years)
          ! approximately min over all cells k and species i of x(i,k)/abs(dxdt_mix + dxdt_burn)
          !log_chem_timescale_div_time_step
          !log_cell_collapse_timescale

      ! integrated power

          !power_h_burn ! total thermal power from PP and CNO, excluding neutrinos (in Lsun units)
          !power_he_burn ! total thermal power from triple-alpha, excluding neutrinos (in Lsun units)
          !power_c_burn ! total thermal power from carbon burning, excluding neutrinos (in Lsun units)
          log_LH ! log10 power_h_burn
          log_LHe ! log10 power_he_burn
          !log_LC ! log10 power_c_burn
          log_LZ ! log10 total burning power including LC, but excluding LH and LHe and photodisintegrations
          log_Lnuc ! log(LH + LHe + LZ)
          !log_Lnuc_sub_log_L
          !extra_L ! integral of extra_heat in Lsun units
          !log_extra_L ! log10 extra_L
          !log_Lneu ! log10 power emitted in neutrinos, nuclear and thermal (in Lsun units)
          !log_Lneu_nuc ! log10 power emitted in neutrinos, nuclear sources only (in Lsun units)
          !log_Lneu_nonnuc ! log10 power emitted in neutrinos, thermal sources only (in Lsun units)
          !mass_loc_of_max_eps_nuc ! (in Msun units)
          !mass_ext_to_max_eps_nuc ! (in Msun units)
          !eps_grav_integral ! (in Lsun units)
          !log_abs_Lgrav ! log10 abs(eps_grav_integral) (in Lsun units)


      ! conditions at the photosphere
          log_Teff ! log10 effective temperature
          !effective_T
          !photosphere_L ! Lsun units
          !photosphere_r ! Rsun units



      ! conditions at or near the surface of the model (outer edge of outer cell)

          !luminosity ! luminosity in Lsun units
          log_L ! log10 luminosity in Lsun units
          log_R ! log10 radius in Rsun units
          !radius ! Rsun
          !radius_cm
          !log_R_cm

          log_g ! log10 gravity
          !gravity
          !log_Ledd
          !log_L_div_Ledd ! log10(L/Leddington)
          !lum_div_Ledd
          !log_surf_opacity
          !log_surf_P
          !log_surf_pressure
          !log_surf_density
          !log_surf_temperature
          !surface_temperature
          log_surf_optical_depth
          !surface_optical_depth
          !log_surf_z

          !surf_avg_j_rot
          !surf_avg_omega
          !surf_avg_omega_crit
          !surf_avg_omega_div_omega_crit
          !surf_avg_v_rot ! km/sec rotational velocity at equator
          !surf_avg_v_crit ! critical rotational velocity at equator
          !surf_avg_v_div_v_crit
          !surf_avg_L_div_Ledd
          !surf_avg_logT
          !surf_avg_logRho
          !surf_avg_opacity

          !surf_escape_v ! cm/s

          !v_wind_Km_per_s ! Km/s
            ! = 1d-5*s% opacity(1)*max(0d0,-s% mstar_dot)/ &
            !        (4*pi*s% photosphere_r*Rsun*s% tau_base)
            ! Lars says:
                ! wind_mdot = 4*pi*R^2*rho*v_wind
                ! tau = integral(opacity*rho*dr) from R to infinity
                ! so tau = opacity*wind_mdot/(4*pi*R*v_wind) at photosphere
                ! or v_wind = opacity*wind_mdot/(4*pi*R*tau) at photosphere

          !rotational_mdot_boost ! factor for increase in mass loss mdot due to rotation
          !log_rotational_mdot_boost ! log factor for increase in mass loss mdot due to rotation
          !surf_r_equatorial_div_r_polar
          !surf_r_equatorial_div_r
          !surf_r_polar_div_r


      ! conditions near center

          log_center_T ! temperature
          log_center_Rho ! density
          log_center_P ! pressure
          !center_T ! temperature
          !center_Rho ! density
          !center_P ! pressure

          !center_degeneracy ! the electron chemical potential in units of k*T
          !center_gamma ! plasma interaction parameter
          center_mu
          center_ye
          center_abar

          !center_eps_grav
          !center_non_nuc_neu
          !center_dL_dm
          !center_eps_nuc
          !d_center_eps_nuc_dlnT
          !d_center_eps_nuc_dlnd
          !log_center_eps_nuc

          !center_entropy ! in units of kerg per baryon
          !max_entropy ! in units of kerg per baryon
          !fe_core_infall
          !non_fe_core_infall

          !compactness_parameter ! (m/Msun)/(R(m)/1000km) for m = 2.5 Msun

          !center_omega
          !center_omega_div_omega_crit


      ! mass fractions near center

          center h1
          center he4
          center c12
          center o16
          ! etc. -- do as many of these 'center' commands as desired

      ! log10 central mass fractions

          !log_center h1
          !log_center he4
          ! etc.


      ! mass fractions near surface

          !surface h1
          !surface he4
          !surface c12
          !surface o16
          ! etc.

      ! log mass fractions near surface

          !log_surface h1
          !log_surface he4

      ! mass fractions for entire star

          !average h1
          !average he4
          ! etc.

      ! mass totals for entire star (in Msun units)

          !total_mass h1
          !total_mass he4
          ! etc.

      ! log10 mass totals for entire star (in Msun units)

          !log_total_mass h1
          !log_total_mass he4
          ! etc.

      ! log10 mass fractions for entire star

          !log_average h1
          !log_average he4
          ! etc.

      ! the following add all of the isos that are in the current net

          ! add_center_abundances
          ! add_surface_abundances
          ! add_average_abundances
          ! add_log_center_abundances
          ! add_log_surface_abundances
          ! add_log_average_abundances


      ! log10 total luminosity for reaction categories (Lsun units)

    !      pp
    !      cno
    !      tri_alfa
    !      burn_c
    !      burn_n
    !      burn_o
    !      burn_ne
    !      burn_na
    !      burn_mg
    !      burn_si
    !      burn_s
    !      burn_ar
    !      burn_ca
    !      burn_ti
    !      burn_cr
    !      burn_fe
    !      c12_c12
    !      c12_o16
    !      o16_o16
    !      photo
    !      pnhe4
    !      other


       ! center log10 burn erg/g/s for reaction categories

          !c_log_eps_burn cno
          !c_log_eps_burn tri_alfa

       ! center d_eps_nuc_dlnd for reaction categories

          !c_d_eps_dlnd cno
          !c_d_eps_dlnd tri_alfa

       ! center d_eps_nuc_dlnT for reaction categories

          !c_d_eps_dlnT cno
          !c_d_eps_dlnT tri_alfa


       ! info about the max burning locations for hydrogen, helium, and metals

          ! info about location where have max rate of hydrogen burning (PP and CNO)
       !max_eps_h ! erg/g/s
       !max_eps_h_lgT ! log10 temperature at location of max burn
       !max_eps_h_lgRho ! log10 density at location of max burn
       !max_eps_h_m ! mass coordinate at location of max burn (Msun units)
       !max_eps_h_xm ! mass exterior to location of max burn (Msun units)
       !max_eps_h_lgP ! log10 pressure at location of max burn
       !max_eps_h_lgR ! log10 radius at location of max burn
       !max_eps_h_opacity ! opacity at location of max burn

       ! info about location where have max rate of helium burning
          ! triple-alpha plus alpha capture on C12, N14, O16, and Ne20.
       !max_eps_he ! erg/g/s
       !max_eps_he_lgT ! log10 temperature at location of max_eps_he
       !max_eps_he_lgRho ! log10 density at location of max burn
       !max_eps_he_m ! mass coordinate at location of max burn (Msun units)
       !max_eps_he_xm ! mass exterior to location of max burn (Msun units)
       !max_eps_he_lgP ! log10 pressure at location of max burn
       !max_eps_he_lgR ! log10 radius at location of max burn
       !max_eps_he_opacity ! opacity at location of max burn

       ! info about location where have max rate of burning of metals
          ! alpha capture on heavy elements plus C+C, C+O, O+O, etc.
       !max_eps_z ! erg/g/s
       !max_eps_z_lgT ! log10 temperature at location of max burn
       !max_eps_z_lgRho ! log10 density at location of max burn
       !max_eps_z_m ! mass coordinate at location of max burn (Msun units)
       !max_eps_z_xm ! mass exterior to location of max burn (Msun units)
       !max_eps_z_lgP ! log10 pressure at location of max burn
       !max_eps_z_lgR ! log10 radius at location of max burn
       !max_eps_z_opacity ! opacity at location of max burn

       ! info about location where have max rate of burning of all types
       !max_eps_nuc ! erg/g/s
       !max_eps_nuc_lgT ! log10 temperature at location of max burn
       !max_eps_nuc_lgRho ! log10 density at location of max burn
       !max_eps_nuc_m ! mass coordinate at location of max burn (Msun units)
       !max_eps_nuc_xm ! mass exterior to location of max burn (Msun units)
       !max_eps_nuc_lgP ! log10 pressure at location of max burn
       !max_eps_nuc_lgR ! log10 radius at location of max burn
       !max_eps_nuc_opacity ! opacity at location of max burn
       !max_eps_nuc_cp ! Cp at location of max burn
       !max_eps_nuc_t_heat ! Cp*T/eps_nuc at location of max burn
       !max_eps_nuc_csound
       !max_eps_nuc_pi_r_div_cs
       max_eps_nuc_H ! pressure scale height
       !max_eps_nuc_H_div_cs
       !max_eps_nuc_log_xa he4 ! any species


     ! info at a specified mass coordinate (given by trace_mass_location)
       !trace_mass_location ! (Msun)
       !trace_mass_radius ! (Rsun)
       !trace_mass_lgT
       !trace_mass_lgRho
       !trace_mass_L ! (Lsun)
       !trace_mass_v

       !trace_mass_lgP
       !trace_mass_g
       !trace_mass_X
       !trace_mass_Y
       !trace_mass_edv_H
       !trace_mass_edv_He
       !trace_mass_scale_height
       !trace_mass_dlnX_dr
       !trace_mass_dlnY_dr
       !trace_mass_dlnRho_dr

       !trace_mass_omega
       !trace_mass_omega_div_omega_crit


     ! info at location of max temperature
       !max_T_lgT
       !max_T_mass ! (Msun)
       !max_T_radius ! (Rsun)
       !max_T_lgRho
       !max_T_lgP
       !max_T_entropy
       !max_T_L ! (Lsun)
       !max_T_eps_nuc ! (erg/g/s)
       !max_T_lgP_thin_shell ! log10(G*Mcore*Menv/(4*pi*Rcore^4))
          ! Mcore = Msun*max_T_mass,
          ! Menv = Msun*(star_mass - max_T_mass),
          ! Rcore = Rsun*max_T_radius
       !max_T_shell_binding_energy ! integral from max_T out

     ! asteroseismology
        !delta_nu ! large frequency separation for p-modes (microHz)
          ! 1e6/(seconds for sound to cross diameter of star)
        !delta_Pg ! g-mode period spacing for l=1 (seconds)
          ! sqrt(2) pi^2/(integral of brunt_N/r dr)
        !log_delta_Pg
        !nu_max ! estimate from scaling relation (microHz)
          ! nu_max = nu_max_sun * M/Msun / ((R/Rsun)^3 (Teff/Teff_sun)^0.5)
          ! with nu_max_sun = 3100 microHz, Teff_sun = 5777
        !nu_max_3_4th_div_delta_nu ! nu_max^0.75/delta_nu
        !acoustic_cutoff ! 0.5*g*sqrt(gamma1*rho/P) at surface
        !acoustic_radius ! integral of dr/csound (seconds)
        !ng_for_nu_max ! = 1 / (nu_max*delta_Pg)
          ! period for g-mode with frequency nu_max = nu_max_ng*delta_Pg
        !gs_per_delta_nu ! delta_nu / (nu_max**2*delta_Pg)
          ! number of g-modes per delta_nu at nu_max

        !int_k_r_dr_nu_max_SL ! integral of k_r*dr where nu < N < Sl for nu = nu_max, l=1
        !int_k_r_dr_2pt0_nu_max_SL ! integral of k_r*dr where nu < N < Sl for nu = nu_max*2, l=1
        !int_k_r_dr_0pt5_nu_max_SL ! integral of k_r*dr where nu < N < Sl for nu = nu_max/2, l=1
        !int_k_r_dr_nu_max_Sl2 ! integral of k_r*dr where nu < N < Sl for nu = nu_max, l=2
        !int_k_r_dr_2pt0_nu_max_Sl2 ! integral of k_r*dr where nu < N < Sl for nu = nu_max*2, l=2
        !int_k_r_dr_0pt5_nu_max_Sl2 ! integral of k_r*dr where nu < N < Sl for nu = nu_max/2, l=2
        !int_k_r_dr_nu_max_Sl3 ! integral of k_r*dr where nu < N < Sl for nu = nu_max, l=3
        !int_k_r_dr_2pt0_nu_max_Sl3 ! integral of k_r*dr where nu < N < Sl for nu = nu_max*2, l=3
        !int_k_r_dr_0pt5_nu_max_Sl3 ! integral of k_r*dr where nu < N < Sl for nu = nu_max/2, l=3



     ! misc

        !v_surf ! (cm/s)
        !v_div_csound_surf ! velocity divided by sound speed at outermost grid point
        !v_surf_div_v_kh ! v_surf/(photosphere_r/kh_timescale)
        !surface_accel_div_grav ! (v - v_old)/dt divided by GM/R^2 at outermost grid point

        !e_thermal ! sum over all zones of Cp*T*dm

        !num_retries ! total during the run
        !num_backups ! total during the run
        !total_num_newton_iterations ! during the run
        !num_newton_iterations ! per step

        !max_conv_vel_div_csound
        !max_gradT_div_grada
        !max_gradT_sub_grada
        !min_log_mlt_Gamma

        !dt_Courant ! min dr_div_csound (sec) -- min cell sound crossing time
        !log_dt_Courant ! log10 min dr_div_csound (sec)
        !dt_Courant_yr ! min dr_div_csound (years)
        !log_dt_Courant_yr ! log10 min dr_div_csound (years)
        !dt_div_dt_Courant
        !log_dt_div_dt_Courant

        !h1_czb_mass ! location (in Msun units) of base of 1st convection zone above he core

        !surf_c12_minus_o16 ! this is useful for seeing effects of dredge up on AGB

        !elapsed_time ! time since start of run (seconds)

        !min_t_eddy ! minimum value of scale_height/conv_velocity

        !min_Pgas_div_P
        !starting_q_min_Pgas_div_P

        !diffusion_solver_steps
        !diffusion_solver_iters

        !version_number ! mesa version from file mesa/data/version_number

        !gradT_excess_alpha
        !gradT_excess_min_beta
        !gradT_excess_max_lambda


        !k_below_Eulerian_eps_grav
        !q_below_Eulerian_eps_grav
        !logxq_below_Eulerian_eps_grav

        !k_Lagrangian_eps_grav
        !q_Lagrangian_eps_grav
        !logxq_Lagrangian_eps_grav

        !k_below_const_q
        !q_below_const_q
        !logxq_below_const_q

        !k_const_mass
        !q_const_mass
        !logxq_const_mass

        !k_below_just_added
        !q_below_just_added
        !logxq_below_just_added

        !k_for_CpTMdot_div_L_limit
        !q_for_CpTMdot_div_L_limit
        !logxq_for_CpTMdot_div_L_limit

        !k_CpTMdot_lt_L
        !q_CpTMdot_lt_L
        !logxq_CpTMdot_lt_L

        !surface_extra_Pgas


        !log_max_T ! temperature
        !max_T