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Common Community Physics Package Developed at DTC
 
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mo_rte_lw Module Reference

Compute longwave radiative fluxes. More...

Functions/Subroutines

character(len=128) function, public rte_lw (optical_props, top_at_1, sources, sfc_emis, fluxes, inc_flux, n_gauss_angles, use_2stream, lw_ds, flux_up_jac)
 
subroutine expand_and_transpose (ops, arr_in, arr_out)
 

Detailed Description

Contains a single routine to compute direct and diffuse fluxes of solar radiation given

  • atmospheric optical properties, spectrally-resolved via one of the sub-classes of [[mo_optical_props(module):ty_optical_props_arry(type)]] in module [[mo_optical_props]]

information about vertical ordering

  • internal Planck source functions, defined per g-point on the same spectral grid at the atmosphere, via [[mo_source_functions(module):ty_source_func_lw(type)]] in module [[mo_source_functions]]

boundary conditions: surface emissivity defined per band

  • optionally, a boundary condition for incident diffuse radiation
  • optionally, an integer number of angles at which to do Gaussian quadrature if scattering is neglected

If optical properties are supplied via class ty_optical_props_1scl (absorption optical thickenss only) ([[mo_optical_props(module):ty_optical_props_1scl(type)]] in module [[mo_optical_props]]) then an emission/absorption solver is called. If optical properties are supplied via class ty_optical_props_2str ([[mo_optical_props(module):ty_optical_props_2str(type)]] in module [[mo_optical_props]]) fluxes are computed via a rescaling by default or, optionally, using two-stream calculations and adding.

Users must ensure that emissivity is on the same spectral grid as the optical properties.

Final output is via user-extensible ty_fluxes ([[mo_fluxes(module):ty_fluxes(type)]] in module [[mo_fluxes]]) which must reduce the detailed spectral fluxes to whatever summary the user needs The routine does error checking and choses which lower-level kernel to invoke based on what kinds of optical properties are supplied