sudo apt-get install gfortran

python setup.py install

>>> import disort
>>> help(disort.run)

performs radiative transfer simulations by means of the DISORT RT solver

Parameters
----------
dTau : array
    optical thickness in atmospheric layers
w0 : float, array
    single scattering albedo (Default: 1.)
iphas : int, array
    scattering phase function type (Default 2).
    1 : Isotropic
    2 : Rayleigh
    3 : Henyey-Greenstein with asymmetry factor GG
    4 : Haze L as specified by Garcia/Siewert
    5 : Cloud C.1 as specified by Garcia/Siewert
6 : Uses user input from Legendre expansion of the phase function uphas
uphas : array, array
    coefficients of first 1000 terms in Legendre polynomial expansion of
    phase function for each layer (Default: [0]*1000)
    (Note this is only required if iphas = 6 for the given layer)
gg : float, array
    scattering asymmetry parameter (Default: 0.85)
umu0 : float
    cosine of solar zenith angle (Default: 1.)
phi0 : float
    solar azimuth angle (Default: 0.)
albedo : float
    surface albedo (Default: 0.1)
fbeam : float
    solar irradiance (Default: 1.)
utau : float, array
    optical thickness where to output the RT fields (Default: 0.)
umu : float, array
    cosine of viewing zenith angle where to output the RT fields (Default: 1.)
phi : float, array
    viewing azimuth angle where to output the RT fields (Default: 0.)
maxmom : int
    Max. number of Legendre coefficients. (Default: 299)
Nstr : int
    Number of computational polar angles to be used
    (= number of 'streams')  ( should be even and .GE. 2 ).
    (Default: 32)
temp : float, array
    LEV = 0 to NLYR, Temperatures (K) of levels.
    (Note that temperature is specified at LEVELS
    rather than for layers.)  Be sure to put top level
    temperature in TEMPER(0), not TEMPER(1).  Top and
    bottom level values do not need to agree with top and
    bottom boundary temperatures (i.e. temperature
    discontinuities are allowed).  (Default: 300.)
wvnmlo, wvnmhi : float
    Wavenumbers (inv cm) of spectral interval of interest
    ( used only for calculating Planck function ).
    Needed only if PLANK is TRUE, or in multiple runs, if
    LAMBER is FALSE and BDREF depends on spectral interval.
    (Default: wvnmlo=999., wvnmhi=1000.)
UsrTau : logical
    = FALSE, Radiant quantities are to be returned
                 at boundary of every computational layer.
    = TRUE,  Radiant quantities are to be returned
                 at user-specified optical depths
    (Default: True)
UsrAng : logical
    = FALSE, Radiant quantities are to be returned
                 at computational polar angles.
    = TRUE,  Radiant quantities are to be returned
                 at user-specified polar angles.
    (Default: True)
ibcnd : int
    = 0, General case: boundary conditions any combination of:
         * beam illumination from the top ( see FBEAM )
         * isotropic illumination from the top ( see FISOT )
         * thermal emission from the top ( see TEMIS, TTEMP )
         * internal thermal emission sources ( see TEMPER )
         * reflection at the bottom ( see LAMBER, ALBEDO, BDREF )
         * thermal emission from the bottom ( see BTEMP )
    = 1, Return only albedo and transmissivity of the entire
         medium vs. incident beam angle; see S2 for details.
    (Default: 0)
fisot : float
    Intensity of top-boundary isotropic illumination.
    [same units as PLKAVG (default W/sq m) if thermal
    sources active, otherwise arbitrary units].
    Corresponding incident flux is pi (3.14159...)
    times FISOT.
    (Default: 0.)
lamber : bool
    = TRUE, isotropically reflecting bottom boundary.
    = FALSE, bidirectionally reflecting bottom boundary.
    (Default: True)
btemp : float
    Temperature of bottom boundary (K)  (bottom emissivity
    is calculated from ALBEDO or function BDREF, so it need
    not be specified). Needed only if PLANK is TRUE.
    (Default: 300.)
ttemp : float
    Temperature of top boundary (K).
    Needed only if PLANK is TRUE.
    (Default: 300.)
temis : float
    Emissivity of top boundary.
    Needed only if PLANK is TRUE.
    (Default: 1.)
plank : bool
    = TRUE,  include thermal emission
    = FALSE, ignore all thermal emission (saves computer time)
    (Default: False)
onlyFl : bool
    = TRUE, return fluxes, flux divergences, and mean
            intensities.
    = FALSE, return fluxes, flux divergences, mean
             intensities, AND intensities.
    (Default: False)
accur : float
    Convergence criterion for azimuthal (Fourier cosine)
    series.  Will stop when the following occurs twice:
    largest term being added is less than ACCUR times
    total series sum.  (Twice because there are cases where
    terms are anomalously small but azimuthal series has
    not converged.)  Should be between 0 and 0.01 to avoid
    risk of serious non-convergence.  Has no effect on
    problems lacking a beam source, since azimuthal series
    has only one term in that case.
    (Default: 0.)
PRNT : array(dtype=bool)
    Array of LOGICAL print flags causing the following prints
       L        quantities printed
      --        ------------------
       1        input variables (except PMOM)
       2        fluxes
       3        intensities at user levels and angles
       4        planar transmissivity and planar albedo
                as a function solar zenith angle ( IBCND = 1 )
       5        phase function moments PMOM for each layer
                ( only if PRNT(1) = TRUE, and only for layers
                with scattering )
    (Default: array([False False False False False]))

Returns
-------
ds_fields : list of arrays
    [rfldir, rfldn, flup, dfdt, uavg, uu, albmed, trnmed]

    rfldir : Downward Direct
    rfldn  : Downward Diffuse
    flup   : Upward Diffuse
    dfdt   : d(Net Flux) / d(Op Dep)
    uu     : Intensity
    uavg   : Mean intensity (including the direct beam)
             (Not corrected for delta-M-scaling effects)
    albmed : Albedo of the medium as a function of incident
             beam angle cosine UMU(IU)  (IBCND = 1 case only)
    trnmed : Transmissivity of the medium as a function of incident
             beam angle cosine UMU(IU)  (IBCND = 1 case only)

Examples
--------
>>> import disort
>>> D_dir, D_diff, U_up, dFdt, I = disort.run(dTau, ssalb, iphas='Rayleigh')