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Host Star Driven Exoplanet Mass Loss and Possible Surface Water

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Host Stars and their Effects on Exoplanet Atmospheres

Part of the book series: Lecture Notes in Physics ((LNP,volume 955))

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Abstract

Whether an exoplanet retains its atmosphere and surface water depends on many factors. I will first describe the two main mass-loss mechanisms for exoplanet atmospheres. The main thermal process is hydrodynamical outflow driven by extreme ultraviolet and x-radiation from the host star that heat and inflate an exoplanet’s exosphere leading to mass loss. Non-thermal mass loss occurs when ions and electrons in the host star’s wind remove neutrals and ions in the exoplanet’s upper atmosphere through charge exchange, ion pick-up, and other processes. Although there are simulations of thermal and non-thermal processes occurring in isolation, these processes can work together to enhance the mass-loss rate. There are, however, many unknowns or poorly known parameters including the exoplanet’s initial water inventory, its orbital migration, the strength of its magnetic field, its outgassing rate, the history of the host star’s UV, EUV and x-radiation, and the present and past flaring and coronal mass ejection (CME) rates. Thus for an exoplanet to be habitable today, it must survive a gauntlet of inadequately known challenges. Latter in the chapter, I describe what the term “habitable zone” is intended to be and include case studies of several exoplanets for which there are estimates of mass loss, surface liquid water, and habitability. Finally, I consider which types of host stars are most likely to support exoplanets that satisfy the wide variety of conditions that appear to be required for habitability.

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Linsky, J. (2019). Host Star Driven Exoplanet Mass Loss and Possible Surface Water. In: Host Stars and their Effects on Exoplanet Atmospheres . Lecture Notes in Physics, vol 955. Springer, Cham. https://doi.org/10.1007/978-3-030-11452-7_10

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