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Types of Hot Jupiter Atmospheres

  • Dmitry V. BisikaloEmail author
  • Pavel V. Kaygorodov
  • Dmitry E. Ionov
  • Valery I. Shematovich
Chapter
Part of the Astrophysics and Space Science Library book series (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.

Keywords

Shock Wave Mass Loss Rate Stellar Wind Contact Discontinuity Lagrangian Point 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Notes

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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Copyright information

© Springer International Publishing Switzerland 2015

Authors and Affiliations

  • Dmitry V. Bisikalo
    • 1
    Email author
  • Pavel V. Kaygorodov
    • 1
  • Dmitry E. Ionov
    • 1
  • Valery I. Shematovich
    • 1
  1. 1.Institute of Astronomy of the Russian Academy of SciencesMoscowRussian Federation

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