Theory and simulation of spectral line broadening by exoplanetary atmospheric haze

TL;DR

This paper presents a comprehensive atomistic model to explain how atmospheric haze causes spectral line broadening and flattening in exoplanetary atmospheres, aiding interpretation of transmission spectra.

Contribution

It introduces a detailed formalism for modeling radiator-haze interactions, accounting for particle structure, size, and composition, improving understanding of spectral line modifications in hazy environments.

Findings

Model explains spectral flattening in hazy atmospheres.

Predicts shifts and broadening of spectral lines due to haze.

Demonstrates application to sodium D line in argon haze.

Abstract

Atmospheric haze is the leading candidate for the flattening of expolanetary spectra, as it's also an important source of opacity in the atmospheres of solar system planets, satellites, and comets. Exoplanetary transmission spectra, which carry information about how the planetary atmospheres become opaque to stellar light in transit, show broad featureless absorption in the region of wavelengths corresponding to spectral lines of sodium, potassium and water. We develop a detailed atomistic model, describing interactions of atomic or molecular radiators with dust and atmospheric haze particulates. This model incorporates a realistic structure of haze particulates from small nano-size seed particles up to sub-micron irregularly shaped aggregates, accounting for both pairwise collisions between the radiator and haze perturbers, and quasi-static mean field shift of levels in haze environments. This formalism can explain large flattening of absorption and emission spectra in haze atmospheres and shows how the radiator - haze particle interaction affects the absorption spectral shape in the wings of spectral lines and near their centers. The theory can account for nearly all realistic structure, size and chemical composition of haze particulates and predict their influence on absorption and emission spectra in hazy environments. We illustrate the utility of the method by computing shift and broadening of the emission spectra of the sodium D line in an argon haze. The simplicity, elegance and generality of the proposed model should make it amenable to a broad community of users in astrophysics and chemistry.