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Planet migration in accretion discs in binary systems

Published online by Cambridge University Press:  16 August 2023

A.D. Nekrasov ,
S.B. Popov Open the ORCID record for S.B. Popov [Opens in a new window]  and
V.V. Zhuravlev
A.D. Nekrasov
Affiliation:
Department of Physics, Lomonosov Moscow State University, 119991, Moscow, Russia Sternberg Astronomical Institute, 119234, Universitetski pr. 13, Moscow, Russia
S.B. Popov
Affiliation:
Department of Physics, Lomonosov Moscow State University, 119991, Moscow, Russia Sternberg Astronomical Institute, 119234, Universitetski pr. 13, Moscow, Russia
V.V. Zhuravlev
Affiliation:
Sternberg Astronomical Institute, 119234, Universitetski pr. 13, Moscow, Russia
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Abstract

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We model evolution of exoplanets of S-type in close binary systems at the stage when the companion starts to lose mass via a slow stellar wind. At this stage an accretion disc is formed around the planets’ host. Detailed structure of such discs is calculated in quasi-stationary and non-stationary approaches. We model migration of planets embedded in these discs.

Keywords

planetary systemsbinaries: closeaccretion disks
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 285 - 286
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Kulikova, O, Popov, S. B., Zhuravlev, V. V., 2019, MNRAS, 487, 3069 10.1093/mnras/stz1363CrossRefGoogle Scholar
Paxton, O., Bildsten, L., Dotter, A., et al., 2011, ApJS, 192, 3 10.1088/0067-0049/192/1/3CrossRefGoogle Scholar
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