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Influence of photoelectrons on the structure and dynamics of the upper atmosphere of a hot Jupiter

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Abstract

A self-consistent, aeronomic model of the upper atmosphere of a “hot Jupiter” including reactions involving suprathermal photoelectrons is presented. This model is used to compute the height profiles of the gas density, velocity, and temperature in the atmosphere of the exoplanet HD 209458b. It is shown that including suprathermal electrons when computing the heating and cooling functions reduces the mass loss rate of the atmosphere by a factor of five.

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Authors and Affiliations

  1. Institute of Astronomy, Russian Academy of Sciences, ul. Pyatnitskaya 48, Moscow, 119017, Russia

    D. E. Ionov, V. I. Shematovich & Ya. N. Pavlyuchenkov

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  1. D. E. Ionov
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  2. V. I. Shematovich
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  3. Ya. N. Pavlyuchenkov
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Correspondence to D. E. Ionov.

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Original Russian Text © D.E. Ionov, V.I. Shematovich, Ya.N. Pavlyuchenkov, 2017, published in Astronomicheskii Zhurnal, 2017, Vol. 94, No. 5, pp. 381–386.

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Ionov, D.E., Shematovich, V.I. & Pavlyuchenkov, Y.N. Influence of photoelectrons on the structure and dynamics of the upper atmosphere of a hot Jupiter. Astron. Rep. 61, 387–392 (2017). https://doi.org/10.1134/S1063772917050018

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  • DOI: https://doi.org/10.1134/S1063772917050018

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