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Types of Hot Jupiter Atmospheres

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Characterizing Stellar and Exoplanetary Environments

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 411))

Abstract

Hot Jupiters, i.e. exoplanet gas giants, having masses comparable to the mass of Jupiter and semimajor axes shorter than 0.1 AU, are a unique class of objects. Since they are so close to the host stars, their atmospheres form and evolve under the action of very active gas dynamical processes caused by the gravitational field and irradiation of the host star. As a matter of fact, the atmospheres of several of these planets fill their Roche lobes , which results in a powerful outflow of material from the planet towards the host star. The energy budget of this process is so important that it almost solely governs the evolution of hot Jupiters gaseous envelopes. Based on the years of experience in the simulations of gas dynamics in mass-exchanging close binary stars, we have investigated specific features of hot Jupiters atmospheres. The analytical estimates and results of 3D numerical simulations, discussed in this Chapter, show that the gaseous envelopes around hot Jupiters may be significantly non-spherical and, at the same time, stationary and long-lived. These results are of fundamental importance for the interpretation of observational data.

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Notes

  1. 1.

    The atmosphere, when expanding, approaches the L1 and L2 points (say, uncork these points) at almost the same time. Thus, hereafter we consider a criterion of corking/uncorking only for the L1 point, keeping in mind that the outflow starts/end through both points.

  2. 2.

    Our assumption that the temperature of the stream is constant all along its trajectory is justified by the fact that the stream and the upper planet’s atmosphere are heated by the radiation of the star in the same way.

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Acknowledgements

The authors acknowledge the support by the International Space Science Institute (ISSI) in Bern, Switzerland and the ISSI team Characterizing stellar- and exoplanetary environments and thank L. Fossati from the Argelander-Institut für Astronomie der Universität Bonn, Germany, Lotfi Ben-Jaffel from the Institut Astrophysique de Paris (IAP) CNRS-UPMC, Paris and Tommi Koskinen from the Lunar and Planetary Laboratory University of Arizona, Tucson, USA for fruitful discussions. The authors also acknowledge the support by the RFBR projects 12-02-00047 and 14-02-00215.

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Authors and Affiliations

  1. Institute of Astronomy of the Russian Academy of Sciences, Moscow, Russian Federation

    Dmitry V. Bisikalo, Pavel V. Kaygorodov, Dmitry E. Ionov & Valery I. Shematovich

Authors
  1. Dmitry V. Bisikalo
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  2. Pavel V. Kaygorodov
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  3. Dmitry E. Ionov
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  4. Valery I. Shematovich
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Correspondence to Dmitry V. Bisikalo .

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Editors and Affiliations

  1. Space Research Institute, Austrian Academy of Sciences, Graz, Austria

    Helmut Lammer

  2. Space Research Institute, Austrian Academy of Sciences, Graz, Austria

    Maxim Khodachenko

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Bisikalo, D.V., Kaygorodov, P.V., Ionov, D.E., Shematovich, V.I. (2015). Types of Hot Jupiter Atmospheres. In: Lammer, H., Khodachenko, M. (eds) Characterizing Stellar and Exoplanetary Environments. Astrophysics and Space Science Library, vol 411. Springer, Cham. https://doi.org/10.1007/978-3-319-09749-7_5

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