Effect of stellar wind induced magnetic fields on planetary obstacles of non-magnetized hot Jupiters
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URI (для ссылок/цитирований):
https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx1471https://elib.sfu-kras.ru/handle/2311/69720
Автор:
Erkaev, N. V.
Odert, P.
Lammer, H.
Kislyakova, K. G.
Fossati, L.
Мезенцев, Александр Владимирович
Johnstone, C. P.
Kubyshkina, D. I.
Shaikhislamov, I. F.
Khodachenko, M. L.
Коллективный автор:
Политехнический институт
Кафедра прикладной механики
Дата:
2017-10Журнал:
Monthly Notices of the Royal Astronomical SocietyКвартиль журнала в Scopus:
Q1Квартиль журнала в Web of Science:
Q1Библиографическое описание:
Erkaev, N. V. Effect of stellar wind induced magnetic fields on planetary obstacles of non-magnetized hot Jupiters [Текст] / N. V. Erkaev, P. Odert, H. Lammer, K. G. Kislyakova, L. Fossati, Александр Владимирович Мезенцев, C. P. Johnstone, D. I. Kubyshkina, I. F. Shaikhislamov, M. L. Khodachenko // Monthly Notices of the Royal Astronomical Society. — 2017. — Т. 470 (№ 4). — С. 4330-4336Аннотация:
We investigate the interaction between themagnetized stellarwind plasma and the partially ionized
hydrodynamic hydrogen outflow from the escaping upper atmosphere of non-magnetized
or weakly magnetized hot Jupiters. We use the well-studied hot Jupiter HD 209458b as an
example for similar exoplanets, assuming a negligible intrinsic magnetic moment. For this
planet, the stellar wind plasma interaction forms an obstacle in the planet’s upper atmosphere,
in which the position of the magnetopause is determined by the condition of pressure balance
between the stellar wind and the expanded atmosphere, heated by the stellar extreme ultraviolet
radiation.We show that the neutral atmospheric atoms penetrate into the region dominated
by the stellar wind, where they are ionized by photoionization and charge exchange, and then
mixed with the stellar wind flow. Using a 3D magnetohydrodynamic (MHD) model, we show
that an induced magnetic field forms in front of the planetary obstacle, which appears to be
much stronger compared to those produced by the solar wind interaction with Venus and
Mars. Depending on the stellar wind parameters, because of the induced magnetic field, the
planetary obstacle can move up to ≈0.5–1 planetary radii closer to the planet. Finally, we
discuss how estimations of the intrinsic magnetic moment of hot Jupiters can be inferred by
coupling hydrodynamic upper planetary atmosphere andMHDstellar wind interaction models
together with UV observations. In particular, we find that HD 209458b should likely have an
intrinsic magnetic moment of 10–20 per cent that of Jupiter.