!*** Radiative transfer (RT) code parameters:
 RTC_TOG = 2   !     2 = RT code based on Toon et al. 1989 (2-stream;
 LONRAD = 1    ! Spatial variation of shortwave radiation  
               !  0 = SW equals that at centlat/lon of coarsest grid (#1)
               !  1 = full dependence on lat/lon on every grid
 ISHADTOG = 1      ! 1 = topo shadowing on all grids, 0 = no shadowing
 LS_OF_PERIAPSE = 250.999    ! Ls of periapse (around the relevant star) [deg]
 ORBITAL_ECCENTRICITY = 0.09341233   ! Eccentricity of body's orbit around star
 AXIAL_OBLIQUITY = 25.1919   ! Obliquity of the body's rotational axis [deg]

 AU_TO_M_KNOB = 1.000085   ! Factor that should be "very nearly" 1; use to
                           !  "coax" the numerical calc of the body's orbit to
                           !  be cyclic (i.e., no orbital calc error messages)
    !=== Control parameters for the output of RT fluxes [f(z,wavelength,stream)]
    !    each RT timestep to separate NetCDF-format files (one per gridpoint;
    !    written to the 'state' directory of the run).
    !    NOTE: Configure this thoughtfully, as this can potentially produce
    !          multiple very large files.
 RT_FLUX_TRACE_NP = 0   ! Number of gridpoints whose information will be written
                !  to file(s);  0 = turn off this feature
    !%%% Start and end times for the writing of information to file:
 @RT_FLUX_TRACE_TI_ = '0. seconds', '1 b_d'
    !%%% Specific gridpoints whose information will be written to individual
    !    files.  Example: 'g01:(12,34)' = grid #1, (x,y) = (12,34) 
 @RT_FLUX_TRACE_PT_ = 'g01:(12,34)','g03:(34,12)'
 DUST_OP_CASE = 3  ! 1 = Palagonite (Ockert-Bell etal. 1997, Clancy etal. 1995)
                   ! 2 = Palagonite (Clancy et al. 1995)
                   ! 3 = Semi-empirical Mars dust (Wolff et al. 2009)
    !=== Control parameters for radiative transfer interaction of FOREGROUND
    !    aerosols (NOTE: water vapor is always radiatively active *if present*):
 DUST_RTA = .FALSE.     ! Dust aerosol is radiatively active?
    !%%% Begin time for inclusion of dust in RT calcs:
 DUST_RTT_ = '0. seconds'
 H2OI_RTA = .FALSE.     ! H2O ice aerosol is radiatively active?
    !%%% Begin time for inclusion of H2O ice_aer in RT calcs:
 H2OI_RTT_ = '0. seconds'
 CO2I_RTA = .FALSE.     ! CO2 ice aerosol is radiatively active?
    !%%% Begin time for inclusion of CO2 ice_aer in RT calcs:
 CO2I_RTT_ = '0. seconds'
  !*** Reference pressure value assumed to correspond to any "background" and
  !     "foreground" dust column opacities that are either specified (i.e.,
  !     BDST_IRT, BDST_ITT, DUST_IRT, DUST_ITT, TAUTOT) or calculated.  It is
  !     strongly suggested that this not be changed from the default value of
  !     610 Pa.  Only in certain special cases will it be beneficial to modify
  !     this, such as when using a surface air pressure that is much different
  !     than that at the present epoch on Mars:
 DUST_CTAU_REFP = 610.   ! [Pa]
  !*** Control parameters for "background" radiatively-active dust scenario
  !     (only "seen" by radTX code; DUST_TOG >= 1 is required):
 BDST_TOG = 4   !  4 = use a f(lat,Ls) prescription based on zonally-averaged
                !       TES MY24 *extinction* tau_9um (natively at 610 Pa; model
                !       will use DUST_CTAU_REFP) and an empirical raster
                !       haze_top field based on SPICAM results, insolation,
                !       etc. {"Mi2008", "vtau"}
       ! Log-normal *number* modal/median/geometric_mean radius [um]
       !   = r_eff/exp(2.5*(rsig)**2) {r_eff = area-weighted effective radius}
       !   = arithmetic_mean*exp(-0.5*rsig**2)
       ! where 'rsig' is the log-normal standard deviation (see BDST_IGD)
 BDST_IMR = 1.5  ! r_eff = 1.5 um (Wolff et al. 2006)
       ! Log-normal number geometric standard deviation (>1.)
       !   = exp(rsig)
       !   = exp(sqrt(log(v_eff+1.)) {v_eff = area-weighted effective variance}
       ! where 'rsig' is the log-normal standard deviation
 BDST_IGD = 1.8  ! v_eff = 0.25 (Wolff et al. 2006)
                    !  (stddev_eff = 0.5; rsig = 0.47238)
  !*** -END- of parameters for "background" radiatively-active dust scenario ***
!*** Aerosol code (with microphysics derived from CARMA) options:
  !*** DUST aerosol: ***---------------------------------------------------
 DUST_TOG = 1      ! Dust:  0 = no dust;
                   !  1 = static profile;
                   !  2 = mobile (sediments, diffuses, advects);
                   !  3 = mobile (#2 AND const stress threshold sfc_source);
                   !  4 = mobile (#2 AND dyn ustar threshold sfc_source);
 DUST_NB = 8    ! Number of separate size/mass bins for dust variables
 DUST_RMN = 5.e-2   ! Minimum particle radius [um]
 DUST_MRT = 7.2    ! Ratio of particle mass between successive bins
    !%%% Time that most dust transport processes (sedimentation, diffusion,
    !    advection) should begin:
 DUST_BEG_ = '35000. seconds'
    !=== ("Foreground") atmospheric dust initialization parameters:
 DUST_IVR = 5   ! Dust aerosol profile initialization override/toggle:
                !  5 = Use a f(lat,Ls) prescription (at the initial time/season)
                !       based on zonally-averaged TES MY24 *extinction* tau_9um
                !       (natively at 610 Pa; model will use DUST_CTAU_REFP) and
                !       an empirical raster haze_top field based on SPICAM
                !       results, insolation, etc. {"Mi2008", "vtau"}
       ! Log-normal number geometric standard deviation (>1.)
       !   = exp(rsig)
       !   = exp(sqrt(log(v_eff+1.)) {v_eff = area-weighted effective variance}
       ! where 'rsig' is the log-normal standard deviation
 DUST_IGD = 1.8  ! v_eff = 0.4127
       ! Log-normal *number* modal/median/geometric_mean radius [um]
       !   = r_eff/exp(2.5*(rsig)**2) {r_eff = area-weighted effective radius}
       !   = arithmetic_mean*exp(-0.5*rsig**2)
       ! where 'rsig' is the log-normal standard deviation (see DUST_IGD)
 DUST_IMR = 1.5   ! r_eff = 3.558 um