Abstract
Exoplanets orbiting close to their parent stars have been observed to lose a fraction of their atmosphere into space: they “evaporate.” The escape of atmospheric gas is due to the large X-ray to ultraviolet (XUV) energy input from the nearby host-star into the upper atmosphere of the planet. Evaporation is characterized through the transit observations of escaping atoms and ions, like hydrogen atoms at Lyman-α, ionized or neutral carbon, oxygen, and magnesium in the UV. Detailed modeling of this phenomenon has to take into account a large number of important physical processes, like the interactions of the upper atmosphere with the stellar environment, radiation pressure, photoionization, self-shielding, charge exchanges, and magnetic interactions with the stellar wind. Massive evaporation can lead some gaseous exoplanets to lose a large fraction of their atmosphere and undergo a significant change in their nature. As a result, some short period, small exoplanets are potentially the remnant of former more massive planets. Evaporation is thus an important process that sculpts the structure of planetary systems with a significant and measurable effect on exoplanets at short orbital distances.
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Acknowledgments
This work has been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). V.B. acknowledges the financial support of the SNSF. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces grant agreement No 724427). A.L. acknowledges support from CNES and the French Agence Nationale de la Recherche (ANR), under programme ANR-12-BS05-0012 “Exo-Atmos.”
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Bourrier, V., Lecavelier des Etangs, A. (2018). Characterizing Evaporating Atmospheres of Exoplanets. In: Deeg, H., Belmonte, J. (eds) Handbook of Exoplanets . Springer, Cham. https://doi.org/10.1007/978-3-319-30648-3_148-1
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