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Modelling the Upper Atmosphere of Gas-Giant Exoplanets Irradiated by Low-Mass Stars pp 1–29Cite as

Introduction

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Part of the book series: Springer Theses ((Springer Theses))

Abstract

The first chapter of this manuscript presents a broad introduction to the subject, including a review of the state of the literature as it was in early 2015, when this thesis was finalised and examined.

This chapter is an enhanced version of a chapter from an original PhD thesis which is available Open Access from the respository https://spiral.imperial.ac.uk/ of Imperial College London. The original chapter was distributed under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (http://creativecommons.org/licenses/by-nc-nd/4.0/), which permits any noncommercial use, duplication, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author and the source, provide a link to the Creative Commons license and indicate if you modified the licensed material. You do not have permission under this license to share adapted material derived from this book or parts of it. The Creative Commence license does not apply to this enhanced chapter, but only to the original chapter of the thesis.

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Notes

  1. 1.

    Note from the author The first chapter of this manuscript presents a broad introduction to the subject, including a review of the state of the literature as it was in early 2015, when this thesis was finalised and examined. Demonstrating the pace of discovery, the number of confirmed exoplanet detections stands at 3610 as of May 2017 (The Extrasolar Planets Encyclopaedia, http://exoplanet.eu Schneider et al. 2011), up from 1890 in May 2015 when this work was examined.

    May 2017.

  2. 2.

    The habitable zone is generally defined as the range of orbital distances over which an Earth-like planet could maintain liquid water at its surface.

  3. 3.

    Throughout this thesis, the following definitions of photon wavebands are used: X-ray (0.517–12.4 nm), Extreme Ultraviolet EUV (12.4–91.2 nm), Far Ultraviolet FUV (\(\sim \)90–200 nm) (unless otherwise specified). XUV is used to refer to the combined X-ray and EUV wavelength ranges.

  4. 4.

    The exobase is the altitude at which the mean free path is equal to the pressure scale height, meaning that the layer above this altitude, the exosphere, is collisionless.

  5. 5.

    The homopause is the boundary between the lower part of the atmosphere where turbulent mixing is dominant—called the homosphere—and higher up in the atmosphere, where molecular diffusion dominates—this is the heterosphere.

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  1. Space Environment Physics, Department of Physics and Astronomy, University of Southampton, Southampton, UK

    Joshua Chadney

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Chadney, J. (2017). Introduction. In: Modelling the Upper Atmosphere of Gas-Giant Exoplanets Irradiated by Low-Mass Stars. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-63351-0_1

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