! log_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 parameter values as of the start of the run
! for completeness, those items are described here:
   
   ! initial_mass -- star mass at start of run (Msun units)
   ! initial_z -- starting metallicity
   ! h1_boundary_limit -- defines abundance limit for h1_boundary_mass 
   ! he4_boundary_limit -- defines abundance limit for he4_boundary_mass
   ! 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
      star_mass ! in Msun units
      !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
   
   ! mixing regions
   
      !  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 using the values defined in const_def
         ! the types are no_mixing, convective_mixing, overshoot_mixing, semiconvective_mixing,
         ! and salt_finger_mixing, numbered from 0 to 4.
         ! 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.

      
   ! 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 m/mstar location of the top of the region
         ! entries for extra columns after the last region in the star will have an invalid value of -9999
         ! 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 '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.
       





   
   ! 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

!     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

      !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

      envelope_mass ! = star_mass - h1_boundary_mass
!     envelope_fraction_left ! = envelope_mass / (initial_mass - h1_boundary_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_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_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)
      !nuc_timescale ! nuclear timescale (years) -- proportional to mass divided by luminosity

   ! integrated power from hydrogen and helium burning
   
      !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)
      log_LH ! log10 power_h_burn
!     log_LHe ! log10 power_he_burn
   
   ! conditions near surface
   
      log_L ! log10 luminosity in Lsun units
      log_Teff ! log10 effective temperature
!     log_R ! log10 radius in Rsun units
!     log_g ! log10 gravity
      !log_L_div_Ledd ! log10(L/Leddington)
   
   ! conditions near center
   
!     log_center_T ! temperature
!     log_center_Rho ! density
!     log_center_P ! pressure
      !center_degeneracy ! the electron chemical potential in units of k*T
      !center_gamma ! plasma interaction parameter
!     center_ye
      !center_entropy ! in kerg units per baryon
      
   ! mass fractions near center
      
!     center h1
!     center he4
!     center c12
!     center o16
      ! etc. -- do as many of these 'center' commands as desired
      
   ! mass fractions near surface
   
       surface h1
       surface he3
      !surface he4
       surface li7
       surface c12
       surface c13
       surface n14
       surface o16
       surface o17
       surface o18
       surface na23
      ! etc.
      
   ! 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.
      
   ! log10 central mass fractions
      
      !log_center h1
      !log_center he4
      ! etc.

   ! log10 total ergs/sec for reaction categories (Lsun units)
      
      pp
      cno
      tri_alfa
      !burn_c
      !burn_n
      !burn_o

   ! log10 total ergs/sec for specific reactions (names from rates_def; Lsun units)
      
      !rpp

   ! info about the max burning locations for hydrogen, helium, and metals
      
      ! info about location where have max rate of hydrogen burning (PP and CNO)
      !eps_h_max ! erg/g/s
      !eps_h_max_lgT ! log10 temperature at location of max burn
      !eps_h_max_lgRho ! log10 density at location of max burn
      !eps_h_max_m ! mass coordinate at location of max burn (Msun units)
      !eps_h_max_lgP ! log10 pressure at location of max burn
      !eps_h_max_lgR ! log10 radius at location of max burn
      !eps_h_max_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.
      !eps_he_max ! erg/g/s
      !eps_he_max_lgT ! log10 temperature at location of max burn
      !eps_he_max_lgRho ! log10 density at location of max burn
      !eps_he_max_m ! mass coordinate at location of max burn (Msun units)
      !eps_he_max_lgP ! log10 pressure at location of max burn
      !eps_he_max_lgR ! log10 radius at location of max burn
      !eps_he_max_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.
      !eps_z_max ! erg/g/s
      !eps_z_max_lgT ! log10 temperature at location of max burn
      !eps_z_max_lgRho ! log10 density at location of max burn
      !eps_z_max_m ! mass coordinate at location of max burn (Msun units)      
      !eps_z_max_lgP ! log10 pressure at location of max burn
      !eps_z_max_lgR ! log10 radius at location of max burn
      !eps_z_max_opacity ! opacity at location of max burn

   
   ! misc
   
!     v_div_csound_surf ! velocity divided by sound speed at outermost grid point
      !surface_accel_div_grav ! (v - v_old)/dt divided by GM/R^2 at outermost grid point
!     num_retries ! total during the run
!     num_backups ! total during the run
      
      !burn_nfcn_total ! only non-zero for burn_split
      !burn_nstep_max ! only non-zero for burn_split
      !lg_nfcn_per_sec ! log10(burn_nfcn_total/dt)
      
      !max_conv_vel_div_csound
      
      !h1_czb_mass ! location (in Msun units) of base of 1st convection zone above h1_boundary_mass
      
      !surf_c12_minus_o16 ! this is useful for seeing effects of dredge up on AGB