2022/08/11 by Quadry Chance, Sarah Ballard, Keivan G. Stassun +1 · 14 citations
Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atmospheric dynamics #Exoplanet #Physics #Stars #Stellar, planetary, and galactic studies
paper · pdf · doi:10.3847/1538-4357/ac8a97
published in The Astrophysical Journal 937(1), 39 (IOP Publishing)
openalex created_date 2020/05/29 · openalex publication_date 2022/09/01 · openalex updated_date 2026/08/05
Abstract The results of large-scale exoplanet transit surveys indicate that the distribution of small planet radii is likely sculpted by atmospheric loss. Several possible physical mechanisms exist for this loss of primordial atmospheres, each of which produces a different set of observational signatures. In this study, we investigate the impact-driven mode of atmosphere loss via N -body simulations. We compare the results from giant impacts, at a demographic level, to results from another commonly invoked method of atmosphere loss, photoevaporation. Applying two different loss prescriptions to the same sets of planets, we then examine the resulting distributions of planets with retained primordial atmospheres. As a result of this comparison, we identify two new pathways toward discerning the dominant atmospheric-loss mechanism at work. Both of these pathways involve using transit multiplicity as a diagnostic, in examining the results of follow-up atmospheric and radial velocity surveys.