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The Evolution of Atmospheric Escape of Highly Irradiated Gassy Exoplanets

Published online by Cambridge University Press:  16 August 2023

Andrew P. Allan Open the ORCID record for Andrew P. Allan [Opens in a new window] ,
Aline A. Vidotto Open the ORCID record for Aline A. Vidotto [Opens in a new window]  and
Leonardo A. Dos Santos Open the ORCID record for Leonardo A. Dos Santos [Opens in a new window]
Andrew P. Allan
Affiliation:
Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
Aline A. Vidotto
Affiliation:
Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
Leonardo A. Dos Santos
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
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Abstract

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Atmospheric escape has traditionally been observed using hydrogen Lyman-α transits, but more recent detections utilise the metastable helium triplet lines at 1083nm. Capable of being observed from the ground, this helium signature offers new possibilities for studying atmospheric escape. Such detections are dependent however on the specific high-energy flux received by the planet. Previous studies show that the extreme-UV band both drives atmospheric escape and populates the triplet state, whereas lower energy mid-UV radiation depopulates the state through photoionisations. This is supported observationally, with the majority of planets with 1083nm detections orbiting a K-type star, which emits a favourably high ratio of EUV to mid-UV flux. The goal of our work is understanding how the observability of escaping helium evolves. We couple our one-dimensional hydrodynamic non-isothermal model of atmospheric escape with a ray-tracing technique to achieve this. We consider the evolution of the stellar radiation and the planet’s gravitational potential.

Keywords

hydrodynamics
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 269 - 274
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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