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A Hydrodynamic Modelling of Atmospheric Escape and Absorption Line of WASP-12b

Published online by Cambridge University Press:  13 January 2020

N. K. Dwivedi Open the ORCID record for N. K. Dwivedi [Opens in a new window] ,
M. L. Khodachenko ,
I. F. Shaikhislamov ,
A. G. Berezutsky ,
I. B. Miroshnichenko ,
L. Fossati ,
H. Lammer ,
Y. Sasunov ,
K. G. Kislyakova Open the ORCID record for K. G. Kislyakova [Opens in a new window]  and
C. P. Johnstone
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N. K. Dwivedi
Affiliation:
Space Research Institute, Austrian Academy of Sciences, Graz, Austria email: [email protected]
M. L. Khodachenko
Affiliation:
Space Research Institute, Austrian Academy of Sciences, Graz, Austria email: [email protected] Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia
I. F. Shaikhislamov
Affiliation:
Institute of Laser Physics, SB RAS, Novosibirsk, Russia
A. G. Berezutsky
Affiliation:
Institute of Laser Physics, SB RAS, Novosibirsk, Russia
I. B. Miroshnichenko
Affiliation:
Institute of Laser Physics, SB RAS, Novosibirsk, Russia
L. Fossati
Affiliation:
Space Research Institute, Austrian Academy of Sciences, Graz, Austria email: [email protected]
H. Lammer
Affiliation:
Space Research Institute, Austrian Academy of Sciences, Graz, Austria email: [email protected]
Y. Sasunov
Affiliation:
Space Research Institute, Austrian Academy of Sciences, Graz, Austria email: [email protected]
K. G. Kislyakova
Affiliation:
Department of Astronomy, University of Vienna, Vienna, Austria
C. P. Johnstone
Affiliation:
Department of Astronomy, University of Vienna, Vienna, Austria
M. Güdel
Affiliation:
Department of Astronomy, University of Vienna, Vienna, Austria
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Abstract

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Self-Consistent 2D modelling of stellar wind interaction with the upper atmosphere of WASP-12b has been performed. The two case-scenarios of the planetary material escape and interaction with the stellar wind, namely the ‘blown by the wind’ (without the inclusion of tidal force) and ‘captured by the star’ (with the tidal force) have been modelled under different stellar XUV radiations and stellar wind parameters. In the first scenario, a shock is formed around the planet, and the planetary mass loss is controlled completely by the stellar radiation energy input. In the second scenario, the mass loss is mainly due to the gravitational interaction effects. The dynamics of MGII and related absorption were modelled with three sets of different stellar wind parameters and XUV flux values.

Keywords

Dynamical evolution and stabilitygaseous planetshot Jupitersetc.
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 301 - 303
Copyright
© International Astronomical Union 2020 

References

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