Тип публикации: статья из журнала
Год издания: 2014
Идентификатор DOI: 10.1088/0004-637X/795/2/132
Ключевые слова: hydrodynamics, planets and satellites: atmospheres, planets and satellites: magnetic fields, planets and satellites: physical evolution, hydrodynamics, planets and satellites: atmospheres, planets and satellites: magnetic fields, planets and satellites: physical evolution
Аннотация: In the present series of papers we propose a consistent description of the mass loss process. To study in a comprehensive way the effects of the intrinsic magnetic field of a close-orbit giant exoplanet (a so-called hot Jupiter) on atmospheric material escape and the formation of a planetary inner magnetosphere, we start with a hydrodynamic model of an upper atmosphere expansion in this paper. While considering a simple hydrogen atmosphere model, we focus on the self-consistent inclusion of the effects of radiative heating and ionization of the atmospheric gas with its consequent expansion in the outer space. Primary attention is paid to an investigation of the role of the specific conditions at the inner and outer boundaries of the simulation domain, under which different regimes of material escape (free and restricted flow) are formed. A comparative study is performed of different processes, such as X-ray and ultraviolet (XUV) heating, material ionization and recombination, H-3(+) cooling, adiabatic and Ly alpha cooling, and Ly alpha reabsorption. We confirm the basic consistency of the outcomes of our modeling with the results of other hydrodynamic models of expanding planetary atmospheres. In particular, we determine that, under the typical conditions of an orbital distance of 0.05AU around a Sun-type star, a hot Jupiter plasma envelope may reach maximum temperatures up to similar to 9000K with a hydrodynamic escape speed of similar to 9 km s(-1), resulting in mass loss rates of similar to(4-7) . 10(10) g s(-1). In the range of the considered stellar-planetary parameters and XUV fluxes, that is close to the mass loss in the energy-limited case. The inclusion of planetary intrinsic magnetic fields in the model is a subject of the follow-up paper (Paper II).
Журнал: ASTROPHYSICAL JOURNAL
Выпуск журнала: Vol. 795, Is. 2
ISSN журнала: 0004637X
Место издания: BRISTOL
Издатель: IOP PUBLISHING LTD
Информация о публикациях загружается с сайта службы поддержки публикационной активности СФУ. Сообщите, если заметили неточности.