PREPRINT
3CBC8D21-0308-4C5A-9780-68A3063FE3CE

Impact of stellar flares on the chemical composition and transmission spectra of gaseous exoplanets orbiting M dwarfs

Thomas Konings, Robin Baeyens, Leen Decin

Submitted on 6 September 2022

Abstract

Stellar flares of active M dwarfs can affect the atmospheric composition of close-orbiting gas giants, and can result in time-dependent transmission spectra. We aim to examine the impact of a variety of flares, differing in energy, duration, and occurrence frequency, on the composition and spectra of close-orbiting, tidally locked gaseous planets with climates dominated by equatorial superrotation. We used a series of pseudo-2D photo- and thermochemical kinetics models, which take advection by the equatorial jet stream into account, to simulate the neutral molecular composition of a gaseous planet (effective temperature 800 K) that orbits a flaring M dwarf. We then computed transmission spectra for the evening and morning limb. We find that the upper regions of the dayside and evening limb are heavily depleted in CH4 and NH3 up to several days after a flare with a total radiative energy of 2×1033 erg. Molar fractions of C2H2 and HCN are enhanced up to a factor three on the nightside and morning limb after day-to-nightside advection of photodissociated species. CH4 depletion reduces transit depths by 100-300 parts per million (ppm) on the evening limb and C2H2 production increases the 14 micron feature up to 350 ppm on the morning limb. We find that repeated flaring drives the atmosphere to a composition that differs from its pre-flare distribution and that this translates to a permanent modification of the transmission spectrum. We show that single high-energy flares can affect the atmospheres of close-orbiting gas giants up to several days after the flare event, during which their transmission spectra are altered by several hundred ppm. Repeated flaring has important implications for future retrieval analyses of exoplanets around active stars, as the atmospheric composition and resulting spectral signatures substantially differ from models that do not include flaring.

Preprint

Comment: 27 pages, 21 figures, accepted for publication in A&A

Subjects: Astrophysics - Earth and Planetary Astrophysics; Astrophysics - Solar and Stellar Astrophysics

URL: https://arxiv.org/abs/2209.02483