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


!# other files

! 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

!----------------------------------------------------------------------------------------------

!# general info about the model

      model_number ! counting from the start of the run
      num_zones ! number of zones in the model

   !## age

      star_age ! elapsed simulated time in years since the start of the run
      !star_age_sec ! elapsed simulated time in seconds since the start of the run
      !star_age_min ! elapsed simulated time in minutes since the start of the run
      !star_age_hr ! elapsed simulated time in hours since the start of the run
      !star_age_day ! elapsed simulated time in days since the start of the run
      !day ! elapsed simulated time in days since the start of the run

      !log_star_age
      !log_star_age_sec

   !## timestep

      !time_step ! timestep in years since previous model
      !time_step_sec ! timestep in seconds since previous model
      !time_step_days
      log_dt ! log10 time_step in years
      !log_dt_sec ! log10 time_step in seconds
      !log_dt_days ! log10 time_step in days

   !## mass

      star_mass ! in Msun units
      !log_star_mass

      !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)

   !## mass change

      !star_mdot ! d(star_mass)/dt (in msolar per year)
      log_abs_mdot ! log10(abs(star_mdot)) (in msolar per year)

   !## imposed surface conditions
      !Tsurf_factor
      !tau_factor
      !tau_surface

   !## imposed center conditions
      !m_center
      !m_center_gm
      !r_center
      !r_center_cm
      !r_center_km
      !L_center
      !log_L_center
      !log_L_center_ergs_s
      !v_center
      !v_center_kms

      !logt_max

!----------------------------------------------------------------------------------------------

!# mixing and convection

      !max_conv_vel_div_csound
      !max_gradT_div_grada
      !max_gradT_sub_grada
      !min_log_mlt_Gamma


   !## 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.
      mixing_regions 20

         ! 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 const/public/const_def.f90.

         ! 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'


   !## 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

!----------------------------------------------------------------------------------------------

!# nuclear reactions

   !## integrated quantities

      !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_photo
      !power_z_burn
      !log_power_nuc_burn ! total thermal power from all burning, excluding photodisintegrations
      log_LH ! log10 power_h_burn
      log_LHe ! log10 power_he_burn
      log_LZ ! log10 total burning power including LC, but excluding LH and LHe and photodisintegrations
      log_Lnuc ! log(LH + LHe + LZ)
      !log_Lnuc_ergs_s
      !log_Lnuc_sub_log_L
      !lnuc_photo

      !extra_L ! integral of extra_heat in Lsun units
      !log_extra_L ! log10 extra_L

   !## neutrino losses
      !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)

   !## information about reactions (by category)

      ! log10 total luminosity for reaction categories (Lsun units)

      pp
      cno
      tri_alpha
      !c_alpha
      !n_alpha
      !o_alpha
      !ne_alpha
      !na_alpha
      !mg_alpha
      !si_alpha
      !s_alpha
      !ar_alpha
      !ca_alpha
      !ti_alpha
      !fe_co_ni
      !c12_c12
      !c12_o16
      !o16_o16
      !photo
      !pnhe4
      !other
   
   !## information about individual reactions
   
          ! adds columns for all of the reactions that are in the current net 
      ! Note that if using op_split_burn=.true. then zones which have been split will report 0 for thier rates
      !add_raw_rates      ! raw reaction rates,       reactions/second
      !add_screened_rates ! screened reaction rates reactions/second
      !add_eps_nuc_rates  ! Nuclear energy (minus neutrino losses) released   erg/s
      !add_eps_neu_rates  ! Neutrino losses             erg/s
   
          ! individual reactions (as many as desired)
          ! use list_net_reactions = .true. in star_job to list all reactions in the current net 
          ! reactions/second
      !raw_rate r_h1_h1_ec_h2 
      !raw_rate r_h1_h1_wk_h2



   !## nuclear reactions at center

      ! 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

   !## 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 20

      !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'
         
      !burn_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 'burn_relr_type_1' and 'burn_relr_top_1'


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

!----------------------------------------------------------------------------------------------

!# information about core and envelope

   !## helium core
      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
      !he_core_k

   !## CO core
      co_core_mass
      !CO_core
      !co_core_radius
      !co_core_lgT
      !co_core_lgRho
      !co_core_L
      !co_core_v
      !co_core_omega
      !co_core_omega_div_omega_crit
      !co_core_k

   !## ONe core
      one_core_mass
      !one_core_radius
      !one_core_lgT
      !one_core_lgRho
      !one_core_L
      !one_core_v
      !one_core_omega
      !one_core_omega_div_omega_crit
      !one_core_k

   !## iron core
      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
      !fe_core_k

   !## neuton rich core
      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
      !neutron_rich_core_k

   !## envelope

      !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
      !co_rich_layer_mass

!----------------------------------------------------------------------------------------------

!# 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

      !dt_cell_collapse ! min time for any cell to collapse at current velocities
      !dt_div_dt_cell_collapse

      !dt_div_max_tau_conv ! dt/ maximum conv timescale
      !dt_div_min_tau_conv ! dt/ minimum conv timescale


      !min_dr_div_cs ! min over all cells of dr/csound (seconds)
      !min_dr_div_cs_k ! location of min
      !log_min_dr_div_cs ! log10 min dr_div_csound (seconds)
      !min_dr_div_cs_yr ! min over all cells of dr/csound (years)
      !log_min_dr_div_cs_yr ! log10 min dr_div_csound (years)
      !dt_div_min_dr_div_cs
      !log_dt_div_min_dr_div_cs

      !min_t_eddy ! minimum value of scale_height/conv_velocity

!----------------------------------------------------------------------------------------------

!# conditions at or near the surface of the model

   !## conditions at the photosphere
      !effective_T
      !Teff
      log_Teff ! log10 effective temperature
         ! Teff is calculated using Stefan-Boltzmann relation L = 4 pi R^2 sigma Teff^4,
         ! where L and R are evaluated at the photosphere (tau_factor < 1)
         ! or surface of the model (tau_factor >= 1) when photosphere is not inside the model.

      !photosphere_black_body_T
      !photosphere_cell_T ! temperature at model location closest to the photosphere, not necessarily Teff
      !photosphere_cell_log_T
      !photosphere_cell_density
      !photosphere_cell_log_density
      !photosphere_cell_opacity
      !photosphere_cell_log_opacity
      !photosphere_L ! Lsun units
      !photosphere_log_L ! Lsun units
      !photosphere_r ! Rsun units
      !photosphere_log_r ! Rsun units
      !photosphere_m ! Msun units
      !photosphere_v_km_s
      !photosphere_cell_k
      !photosphere_column_density
      !photosphere_csound
      !photosphere_log_column_density
      !photosphere_opacity
      !photosphere_v_div_cs
      !photosphere_xm
      !photosphere_cell_free_e
      !photosphere_cell_log_free_e
      !photosphere_logg
      !photosphere_T

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

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

      log_g ! log10 gravity
      !gravity
      !log_Ledd
      !log_L_div_Ledd ! log10(L/Leddington)
      !lum_div_Ledd
      !log_surf_optical_depth
      !surface_optical_depth

      !log_surf_cell_opacity ! old name was log_surf_opacity
      !log_surf_cell_P ! old name was log_surf_P
      !log_surf_cell_pressure ! old name was log_surf_pressure
      !log_surf_cell_density ! old name was log_surf_density
      !log_surf_cell_temperature ! old name was log_surf_temperature
      !surface_cell_temperature ! old name was surface_temperature
      !log_surf_cell_z ! old name was log_surf_z
      !surface_cell_entropy ! in units of kerg per baryon
          ! old name was surface_entropy

      !v_surf ! (cm/s)
      !v_surf_km_s ! (km/s)
      v_div_csound_surf ! velocity divided by sound speed at outermost grid point
      !v_div_csound_max ! max value of velocity divided by sound speed at face
      !v_div_vesc
      !v_phot_km_s
      !v_surf_div_escape_v

      !v_surf_div_v_kh ! v_surf/(photosphere_r/kh_timescale)

      !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_Lrad_div_Ledd
      !surf_avg_logT
      !surf_avg_logRho
      !surf_avg_opacity

      ! Gravity Darkening, reports the surface averaged L/Lsun and Teff (K) caused by
      ! gravity darkening in rotating stars. Based on the model of Espinosa Lara & Rieutord (2011)
      ! 'polar' refers to the line of sight being directed along the rotation axis of the star
      ! 'equatorial' refers to the line of sight coincident with the stellar equator
      !grav_dark_L_polar !Lsun 
      !grav_dark_Teff_polar !K
      !grav_dark_L_equatorial !Lsun 
      !grav_dark_Teff_equatorial !K

      !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

      ! shorter names for above
      log_cntr_P
      log_cntr_Rho
      log_cntr_T

      !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_zbar

      !center_eps_grav

      !center_non_nuc_neu
      !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
      !non_fe_core_rebound
      !max_infall_speed

      !compactness_parameter ! (m/Msun)/(R(m)/1000km) for m = 2.5 Msun
      !compactness
      !m4 ! Mass co-ordinate where entropy=4
      ! mu4 is sensitive to the choice of how much dm/dr you average over, thus we average dm and dr over M(entropy=4) and M(entropy=4)+0.3Msun
      !mu4 ! dM(Msun)/dr(1000km) where entropy=4


      !center_omega
      !center_omega_div_omega_crit

!----------------------------------------------------------------------------------------------

!# abundances

      !species ! size of net

   !## mass fractions near center

      ! the following controls automatically add columns for all of the isos that are in the current net
      !add_center_abundances
      !add_log_center_abundances

      ! individual central mass fractions (as many as desired)
      center h1
      center he4
      center c12
      center o16

      ! individual log10 central mass fractions (as many as desired)
      !log_center h1
      !log_center he4
      ! etc.


   !## mass fractions near surface

      ! the following controls automatically add columns for all of the isos that are in the current net
      !add_surface_abundances
      !add_log_surface_abundances

      ! individual surface mass fractions (as many as desired)
      !surface h1
      !surface he4
      surface c12
      surface o16
      ! etc.

      ! individual log10 surface mass fractions (as many as desired)

      !log_surface h1
      !log_surface he4


   !## mass fractions for entire star

      ! the following controls automatically add columns for all of the isos that are in the current net
      !add_average_abundances
      !add_log_average_abundances

      ! individual average mass fractions (as many as desired)
      !average h1
      !average he4
      ! etc.

      ! individual log10 average mass fractions (as many as desired)
      !log_average h1
      !log_average he4
      ! etc.


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

      ! the following controls automatically add columns for all of the isos that are in the current net
      !add_total_mass
      !add_log_total_mass

      ! individual mass totals for entire star (as many as desired)
      total_mass h1
      total_mass he4
      ! etc.

      ! individial log10  mass totals for entire star (in Msun units)
      !log_total_mass h1
      !log_total_mass he4
      ! etc.

!----------------------------------------------------------------------------------------------

!# info at specific locations
      
   !## info at location of max temperature
   !max_T
   !log_max_T


!----------------------------------------------------------------------------------------------

!# information about shocks

   !## info about outermost outward moving shock
      ! excluding locations with q > max_q_for_outer_mach1_location
      ! returns values at location of max velocity
      !shock_mass ! baryonic (Msun)
      !shock_mass_gm ! baryonic (grams)
      !shock_q
      !shock_radius ! (Rsun)
      !shock_radius_cm ! (cm)
      !shock_velocity
      !shock_csound
      !shock_v_div_cs
      !shock_lgT
      !shock_lgRho
      !shock_lgP
      !shock_gamma1
      !shock_entropy
      !shock_tau
      !shock_k
      !shock_pre_lgRho

!----------------------------------------------------------------------------------------------

!# 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)^2 (Teff/astero_Teff_sun)^0.5)
      !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_Sl1 ! integral of k_r*dr where nu < N < Sl for nu = nu_max, l=1
      !int_k_r_dr_2pt0_nu_max_Sl1 ! integral of k_r*dr where nu < N < Sl for nu = nu_max*2, l=1
      !int_k_r_dr_0pt5_nu_max_Sl1 ! 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

!----------------------------------------------------------------------------------------------

!# energy information

      !total_energy ! at end of step
      !log_total_energy ! log(abs(total_energy))
      !total_energy_after_adjust_mass ! after mass adjustments

      ! shorter versions of above
      !tot_E
      !log_tot_E


      !total_gravitational_energy
      !log_total_gravitational_energy ! log(abs(total_gravitational_energy))
      !total_gravitational_energy_after_adjust_mass

      ! shorter versions of above
      !tot_PE
      !log_tot_PE

      !total_internal_energy
      !log_total_internal_energy
      !total_internal_energy_after_adjust_mass

      ! shorter versions of above
      !tot_IE
      !log_tot_IE

      !total_radial_kinetic_energy
      !log_total_radial_kinetic_energy
      !total_radial_kinetic_energy_after_adjust_mass

      ! shorter versions of above (does not include rot KE)
      !tot_KE
      !log_tot_KE

      !total_turbulent_energy
      !log_total_turbulent_energy
      !total_turbulent_energy_after_adjust_mass
      !tot_Et
      !log_tot_Et

      !total_energy_foe

      !tot_IE_div_IE_plus_KE
      !total_IE_div_IE_plus_KE

      !total_entropy
      !total_eps_grav

      !total_energy_sources_and_sinks ! for this step
      !total_nuclear_heating
      !total_non_nuc_neu_cooling
      !total_irradiation_heating
      !total_extra_heating ! extra heat integrated over the model times dt (erg)
      !total_WD_sedimentation_heating

      !rel_run_E_err

      !rel_E_err
      !abs_rel_E_err
      !log_rel_E_err

      !tot_e_equ_err
      !tot_e_err


      !error_in_energy_conservation ! for this step
         ! = total_energy - (total_energy_start + total_energy_sources_and_sinks)
      !cumulative_energy_error ! = sum over all steps of abs(error_in_energy_conservation)
      !rel_cumulative_energy_error ! = cumulative_energy_error/total_energy
      !log_rel_cumulative_energy_error ! = log10 of rel_cumulative_energy_error
      !log_rel_run_E_err ! shorter name for rel_cumulative_energy_error

      !rel_error_in_energy_conservation ! = error_in_energy_conservation/total_energy
      !log_rel_error_in_energy_conservation

      !virial_thm_P_avg
      !virial_thm_rel_err
      !work_inward_at_center
      !work_outward_at_surface


!----------------------------------------------------------------------------------------------

 !# rotation

      !total_angular_momentum
      !log_total_angular_momentum
      !i_rot_total ! moment of inertia

      !total_rotational_kinetic_energy
      !log_total_rotational_kinetic_energy
      !total_rotational_kinetic_energy_after_adjust_mass

!----------------------------------------------------------------------------------------------

!# velocities

      !avg_abs_v_div_cs
      !log_avg_abs_v_div_cs
      !max_abs_v_div_cs
      !log_max_abs_v_div_cs

      !avg_abs_v
      !log_avg_abs_v
      !max_abs_v
      !log_max_abs_v

      !u_surf
      !u_surf_km_s
      !u_div_csound_surf
      !u_div_csound_max

      !infall_div_cs

!----------------------------------------------------------------------------------------------

!# misc

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

   !## eos
      !logQ_max ! logQ = logRho - 2*logT + 12
      !logQ_min
      !gamma1_min

   !## core mixing
      !mass_semiconv_core

   !## H-He boundary

      !diffusion_time_H_He_bdy
      !temperature_H_He_bdy


   !## optical depth and opacity

      !one_div_yphot
      !log_one_div_yphot

      !log_min_opacity
      !min_opacity

      !log_tau_center

      !log_max_tau_conv
      !max_tau_conv
      !log_min_tau_conv
      !min_tau_conv

      !tau_qhse_yrs

   !## other

      !Lsurf_m
      !dlnR_dlnM
      !h1_czb_mass ! location (in Msun units) of base of 1st convection zone above he core
      !kh_mdot_limit
      !log_cntr_dr_cm
      !min_Pgas_div_P
      !surf_c12_minus_o16 ! this is useful for seeing effects of dredge up on AGB
      !surf_num_c12_div_num_o16

      !phase_of_evolution ! Integer mapping to the type of evolution see star_data/public/star_data_def.inc for definitions

   !## MLT++
      !gradT_excess_alpha
      !gradT_excess_min_beta
      !gradT_excess_max_lambda

      !max_L_rad_div_Ledd
      !max_L_rad_div_Ledd_div_phi_Joss


   !## RTI
      !rti_regions <num>

   !## Ni & Co
      !total_ni_co_56


   !## internal structure constants

      ! this is evaluated assuming a spherical star and does not account for rotation
      !apsidal_constant_k2


!----------------------------------------------------------------------------------------------

!# accretion

      !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_test_CpT_absMdot_div_L
      !q_for_test_CpT_absMdot_div_L
      !logxq_for_test_CpT_absMdot_div_L

!----------------------------------------------------------------------------------------------

!# Color output

      ! Outputs the bolometric correction (bc) for the star in filter band ``filter'' (case sensitive)
      !bc filter

      ! Outputs the absolute magnitude for the star in filter band ``filter'' (case sensitive)
      !abs_mag filter

      ! Adds all the bc's to the output
      !add_bc

      ! Adds all the absolute magnitudes to the output
      !add_abs_mag

      ! Outputs luminosity in filter band ``filter'' (erg s^-1) (case sensitive)
      ! lum_band filter

      ! Adds all the filter band luminosities to the output (erg s^-1)
      ! add_lum_band

      ! Outputs log luminosity in filter band ``filter'' (log erg s^-1) (case sensitive)
      ! log_lum_band filter

      ! Adds all the filter band luminosities to the output (log erg s^-1)
      ! add_log_lum_band

!----------------------------------------------------------------------------------------------

!# RSP

   !rsp_DeltaMag ! absolute magnitude difference between minimum and maximum light (mag)
   !rsp_DeltaR ! R_max - R_min difference in the max and min radius (Rsun)
   !rsp_GREKM ! fractional growth of the kinetic energy per pulsation period ("nonlinear growth rate") - see equation 5 in MESA5
   !rsp_num_periods ! Count of the number of pulsation cycles completed
   !rsp_period_in_days ! Running period, ie., period between two consecutive values of R_max (days) 
   !rsp_phase ! Running pulsation phase for a cycle

!----------------------------------------------------------------------------------------------
!# debugging

   !## retries
      num_retries ! total during the run

   !## solver iterations

      num_iters ! same as num_solver_iterations
      !num_solver_iterations ! iterations at this step
      !total_num_solver_iterations ! total iterations during the run
      !avg_num_solver_iters

      !rotation_solver_steps

      !diffusion_solver_steps
      !diffusion_solver_iters

      !avg_setvars_per_step
      !avg_skipped_setvars_per_step
      !avg_solver_setvars_per_step

      !burn_solver_maxsteps

      !total_num_solver_calls_converged
      !total_num_solver_calls_failed
      !total_num_solver_calls_made
      !total_num_solver_relax_calls_converged
      !total_num_solver_relax_calls_failed
      !total_num_solver_relax_calls_made
      !total_num_solver_relax_iterations

      !total_step_attempts
      !total_step_redos
      !total_step_retries
      !total_steps_finished
      !total_steps_taken

      !TDC_num_cells

   !## Relaxation steps
      !total_relax_step_attempts
      !total_relax_step_redos
      !total_relax_step_retries
      !total_relax_steps_finished
      !total_relax_steps_taken

   !## conservation during mesh adjust
      !log_mesh_adjust_IE_conservation
      !log_mesh_adjust_KE_conservation
      !log_mesh_adjust_PE_conservation

   !## amr
      !num_hydro_merges
      !num_hydro_splits

   !## timing
      !elapsed_time ! time since start of run (seconds)
