Кл.слова (ненормированные):
planet-star interactions -- planets and satellites: atmospheres -- planets and satellites: terrestrial planets -- 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. © 2015. The American Astronomical Society. All rights reserved.
Scopus,
WOS
Держатели документа:
University of Vienna, Department of Astrophysics, Vienna, Austria
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
Institute for Computational Modelling, Siberian Division, Russian Academy of Sciences, Krasnoyarsk, Russian Federation
Siberian Federal University, Krasnoyarsk, Russian Federation
Доп.точки доступа:
Johnstone, C. P.; Gudel, M.; Stokl, A. ; Lammer, H.; Tu, L.; Kislyakova, K. G.; Luftinger, T.; Odert, P.; Erkaev, N.V.; Еркаев, Николай Васильевич; Dorfi, E. A.
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