Analytical Models of Exoplanetary Atmospheres. II. Radiative Transfer via the Two-stream Approximation

TL;DR

This paper develops analytical models for exoplanetary atmospheres using the two-stream approximation, incorporating non-isotropic scattering, and provides solutions for temperature-pressure profiles, albedos, and radiative fluxes.

Contribution

It introduces a comprehensive formalism for two-stream radiative transfer including non-isotropic scattering and derives new analytical solutions for atmospheric profiles and radiative properties.

Findings

Hemisphere closure naturally derives from energy conservation.

Eddington closure causes spurious enhancements in reflected and emitted light.

Optical depth of the photosphere depends on multiple factors beyond Milne's 2/3 value.

Abstract

We present a comprehensive analytical study of radiative transfer using the method of moments and include the effects of non-isotropic scattering in the coherent limit. Within this unified formalism, we derive the governing equations and solutions describing two-stream radiative transfer (which approximates the passage of radiation as a pair of outgoing and incoming fluxes), flux-limited diffusion (which describes radiative transfer in the deep interior) and solutions for the temperature-pressure profiles. Generally, the problem is mathematically under-determined unless a set of closures (Eddington coefficients) is specified. We demonstrate that the hemispheric (or hemi-isotropic) closure naturally derives from the radiative transfer equation if energy conservation is obeyed, while the Eddington closure produces spurious enhancements of both reflected light and thermal emission. We concoct recipes for implementing two-stream radiative transfer in stand-alone numerical calculations and general circulation models. We use our two-stream solutions to construct toy models of the runaway greenhouse effect. We present a new solution for temperature-pressure profiles with a non-constant optical opacity and elucidate the effects of non-isotropic scattering in the optical and infrared. We derive generalized expressions for the spherical and Bond albedos and the photon deposition depth. We demonstrate that the value of the optical depth corresponding to the photosphere is not always 2/3 (Milne's solution) and depends on a combination of stellar irradiation, internal heat and the properties of scattering both in optical and infrared. Finally, we derive generalized expressions for the total, net, outgoing and incoming fluxes in the convective regime.