Сибирский федеральный университет

Тип публикации: статья из журнала

Год издания: 2015

Идентификатор DOI: 10.1088/2041-8205/815/1/L12

Ключевые слова: planets and satellites: atmospheres, planets and satellites: terrestrial planets, planet-star interactions, stars: activity, stars: low-mass, stars: rotation

Аннотация: Terrestrial planets formed within gaseous protoplanetary disks can accumulate significant hydrogen envelopes. The evolution of such an atmosphere due to XUV driven evaporation depends on the activity evolution of the host star, which itself depends sensitively on its rotational evolution, and therefore on its initial rotation rate. In this Letter, we derive an easily applicable method for calculating planetary atmosphere evaporation that combines models for a hydrostatic lower atmosphere and a hydrodynamic upper atmosphere. We show that the initial rotation rate of the central star is of critical importance for the evolution of planetary atmospheres and can determine if a planet keeps or loses its primordial hydrogen envelope. Our results highlight the need for a detailed treatment of stellar activity evolution when studying the evolution of planetary atmospheres.

Журнал: ASTROPHYSICAL JOURNAL LETTERS

Выпуск журнала: Vol. 815, Is. 1

ISSN журнала: 20418205

Место издания: BRISTOL

Издатель: IOP PUBLISHING LTD

• Johnstone C.P. (University of Vienna,Department of Astrophysics)
• Erkaev N.V. (Siberian Federal University)
• Gudel M. (University of Vienna,Department of Astrophysics)
• Stokl A. (University of Vienna,Department of Astrophysics)
• Tu L. (University of Vienna,Department of Astrophysics)
• Luftinger T. (University of Vienna,Department of Astrophysics)
• Dorfi E.A. (University of Vienna,Department of Astrophysics)
• Lammer H. (Space Research Institute,Austrian Academy of Sciences)
• Kislyakova K.G. (Space Research Institute,Austrian Academy of Sciences)
• Odert P. (Space Research Institute,Austrian Academy of Sciences)

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