Doppler-Shifted Alkali D Absorption as Indirect Evidence for Exomoons

TL;DR

This paper explores how Doppler-shifted alkali absorption lines in exoplanet atmospheres can serve as indirect evidence for exomoons, emphasizing the role of exomoon-magnetosphere interactions and Doppler effects in detection.

Contribution

It introduces the idea that Doppler shifts and alkali absorption features can indicate exomoons, proposing a mechanism involving exomoon-magnetosphere interactions similar to Io-Jupiter.

Findings

Radiation pressure influences alkali gas dynamics in close-orbiting exoplanets.

Doppler shifts can help isolate planetary signatures from stellar absorption.

Energetic sodium Doppler structures are promising exomoon indicators.

Abstract

Sodium and potassium signatures in transiting exoplanets can be challenging to isolate from the stellar absorption lines. Here, these challenges are discussed in the framework of Solar System observations, and transits of Mercury in particular. Radiation pressure is important for alkali gas dynamics in close-orbiting exoplanets since the D lines are efficient at resonant scattering. When the star-planet velocity is >10km/s, eccentric exoplanets experience more than an order of magnitude higher radiation pressures, aiding atmospheric escape and producing a larger effective cross-section for absorbing starlight at the phase of transit. The Doppler shift also aids in isolating the planetary signature from the stellar photosphere's absorption. Only one transiting exoplanet, HD 80606b, is presently thought to have both this requisite Doppler shift and alkali absorption. Radiation pressure on a planetary exosphere naturally produces blue-shifted absorption, but at levels insufficient to account for the extreme Doppler shifts that have been inferred from potassium transit measurements of this system. In the absence of clear mechanisms to generate such a strong wind, it is described how this characteristic could arise from an exomoon-magnetosphere interaction, analogous to Io-Jupiter. At low contrasts presented here, follow-up transit spectra of HD 80606b cannot rule out a potassium jet or atmospheric species with a broad absorption structure. However, it is evident that line absorption within the imaging passbands fails to explain the narrow-band photometry that has been reported in-transit. New observations of energetic alkalis produced by the Io-Jupiter interaction are also presented, which illustrate that energetic sodium Doppler structure offers a more valuable marker for the presence of an exomoon than potassium.