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Exoplanet Upper Atmosphere Environment Characterization

Published online by Cambridge University Press:  23 April 2012

Helmut Lammer
Affiliation:
Austrian Academy of Sciences, Space Research Institute Schmiedlstr. 6, A-8042, Graz, Austria email: helmut.lammer@oeaw.ac.at, maxim.khodachenko@oeaw.ac.at
Kristina G. Kislyakova
Affiliation:
N.I. Lobachevsky State University, University of Nizhnij Novgorod, 23 Prospekt Gagarina, 603950 Nizhnij Novgorod, Russian Federation email: kislyakova.kristina@gmail.com Institute for Physics/IGAM, University of Graz, Universitätsplatz 5, 8010 Graz, Austria email: petra.odert@uni-graz.at, martin.leitzinger@uni-graz.at, arnold.hanslmeier@uni-graz.at
Petra Odert
Affiliation:
Institute for Physics/IGAM, University of Graz, Universitätsplatz 5, 8010 Graz, Austria email: petra.odert@uni-graz.at, martin.leitzinger@uni-graz.at, arnold.hanslmeier@uni-graz.at
Martin Leitzinger
Affiliation:
Institute for Physics/IGAM, University of Graz, Universitätsplatz 5, 8010 Graz, Austria email: petra.odert@uni-graz.at, martin.leitzinger@uni-graz.at, arnold.hanslmeier@uni-graz.at
Maxim L. Khodachenko
Affiliation:
Austrian Academy of Sciences, Space Research Institute Schmiedlstr. 6, A-8042, Graz, Austria email: helmut.lammer@oeaw.ac.at, maxim.khodachenko@oeaw.ac.at
Mats Holmström
Affiliation:
Swedish Institute of Space Physics, Box 812, SE-98128 Kiruna, Sweden email: matsh@irf.se
Arnold Hanslmeier
Affiliation:
Institute for Physics/IGAM, University of Graz, Universitätsplatz 5, 8010 Graz, Austria email: petra.odert@uni-graz.at, martin.leitzinger@uni-graz.at, arnold.hanslmeier@uni-graz.at
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Abstract

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The intense stellar SXR and EUV radiation exposure at “Hot Jupiters” causes profound responses to their upper atmosphere structures. Thermospheric temperatures can reach several thousands of Kelvins, which result in dissociation of H2 to H and ionization of H to H+. Depending on the density and orbit location of the exoplanet, as a result of these high temperatures the thermosphere expands dynamically up to the Roche lobe, so that geometric blow-off with large mass loss rates and intense interaction with the stellar wind plasma can occur. UV transit observations together with advanced numerical models can be used to gain knowledge on stellar plasma and the planet's magnetic properties, as well as the upper atmosphere.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

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