Theory and simulation of spectral line broadening by exoplanetary atmospheric 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.

Formation of argon cluster with proton seeding

“…Recent interest in optical and physical properties of gas phase clusters has been partly stimulated by discovery of exoplanets and analysis of absorption and emission spectra of their hazy atmospheres. Optical and infrared spectra observed from planetary and exoplanetary atmospheres, comets, and natural satellites are sometimes unusually featureless, which are attributed to the presence of atmospheric dust, ice, haze and aerosol particles [5][6][7]. Haze is mostly formed by small (submicron) cluster particulates that can produce a broad continuum opacity to light.…”

“…The potential energy between argon atoms and protons (blue) is defined in short (I), and long (III) ranges, with a switching function connecting them in region (II), Eqs. (2)-(5).…”

“…Haze is mostly formed by small (submicron) cluster particulates that can produce a broad continuum opacity to light. Interaction between haze particles and radiating atoms or molecules can dramatically modify absorption spectra of exoplanets [5,[8][9][10][11] and used as markers for simulation of atmospheric constituents. Recent laboratory experiments simulating hazy environments for super-Earths and mini-Neptunes atmospheres suggest that some of these atmospheres contain thick photochemically generated hazes [12].…”