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Kinetic Model of the Effect of the Stellar Wind on the Extended Hydrogen Atmosphere of the Exoplanet π Men c

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Abstract

In this work, the kinetic model of aeronomy of the upper atmosphere of an exoplanet is extended by including the effect of stellar wind plasma on the extended hydrogen corona of a hot sub-Neptune. For this purpose, the precipitation of high-energy protons and hydrogen atoms into planetary atmospheres was studied using previously developed kinetic Monte Carlo models. The kinetic model was adapted to the upper atmospheres of hot sub-Neptunes, which made it possible to calculate the energy deposition rate of stellar wind plasma in the planetary corona and to refine estimates of the rate of non-thermal loss of the atmosphere caused by the stellar wind of the parent star. Calculations carried out for the hot sub-Neptune π Men c showed that the energy of the flux of energetic neutral hydrogen atoms (ENA H) penetrating into the atmosphere, formed during the charge exchange of stellar wind protons with thermal atoms of the hydrogen corona, mainly goes to heating the hydrogen corona of the hot exoplanet.

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Funding

This work was supported by the Russian Science Foundation, project no. 22-22-00909.

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Authors and Affiliations

  1. Institute of Astronomy, Russian Academy of Sciences, 119017, Moscow, Russia

    A. A. Avtaeva & V. I. Shematovich

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  1. A. A. Avtaeva
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  2. V. I. Shematovich
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Correspondence to A. A. Avtaeva.

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Translated by E. Chernokozhin

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Avtaeva, A.A., Shematovich, V.I. Kinetic Model of the Effect of the Stellar Wind on the Extended Hydrogen Atmosphere of the Exoplanet π Men c. Astron. Rep. 67, 979–990 (2023). https://doi.org/10.1134/S1063772923100025

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  • DOI: https://doi.org/10.1134/S1063772923100025

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