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The Atmospheric Wind of Hot Exoplanets and its Manifestations in Observations: from Energy Estimates to 3D MHD Models

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Abstract—

The studies of close-orbit gaseous exoplanets—hot Jupiters and warm Neptunes—are reviewed. Transit spectral observations of the Hubble Space Telescope stimulated the numerical modeling of these objects. The supersonic outflow of the upper atmosphere of hot exoplanets and its interaction with the stellar plasma flow is a newly-discovered phenomenon in plasma physics and astrophysics that pools photo- and plasma-chemistry, collision-induced gas-dynamics, and collisionless space plasma. Starting from 2003, the modeling of physical processes in this field has considerably developed from simple quasi-empiric analytical formulas to global three-dimensional magnetic hydrodynamic (3D MHD) codes. The attained level makes it possible to interpret the in-transit measurements in absorption lines of different elements and estimate the parameters of both the planetary atmospheres and the stellar plasma wind.

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Funding

The review was prepared under the support of the Russian Foundation for Basic Research (project no. 19-12-50043). The authors’ studies, which yielded the results reported here, were supported by the Russian Scientific Foundation (project no. 18-12-00080) and the Russian Foundation for Basic Research (project nos. 20-02-00520-а, 16-52-14006-anf).

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Authors and Affiliations

  1. Institute of Laser Physics, Siberian Branch, Russian Academy of Sciences, 630090, Novosibirsk, Russia

    I. F. Shaikhislamov & A. G. Berezutskiy

  2. Institut für Weltraumforschung (Space Research Institute), Austrian Academy of Sciences, Graz, Austria

    M. L. Khodachenko

Authors
  1. I. F. Shaikhislamov
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  2. M. L. Khodachenko
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  3. A. G. Berezutskiy
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Correspondence to I. F. Shaikhislamov.

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Translated by E. Petrova

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Shaikhislamov, I.F., Khodachenko, M.L. & Berezutskiy, A.G. The Atmospheric Wind of Hot Exoplanets and its Manifestations in Observations: from Energy Estimates to 3D MHD Models. Astron. Rep. 65, 8–25 (2021). https://doi.org/10.1134/S1063772921010054

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  • DOI: https://doi.org/10.1134/S1063772921010054

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