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/ C. P. Johnstone [et al.] // Astrophys. J. Lett. - 2015. - Vol. 815, Is. 1, DOI 10.1088/2041-8205/815/1/L12 . - ISSN 2041-8205
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.

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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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/ K. G. Kislyakova [et al.] // Mon. Not. R. Astron. Soc. - 2016. - Vol. 461, Is. 1. - P988-999, DOI 10.1093/mnras/stw1110 . - ISSN 0035-8711
Аннотация: We suggest an additional possible plasma source to explain part of the phenomena observed for the transiting hot Jupiters WASP-12b and HD 189733b in their ultraviolet (UV) light curves. In the proposed scenario, material outgasses from the molten surface of Trojan satellites on tadpole orbits near the Lagrange points L4 and L5. We show that the temperature at the orbital location of WASP-12b is high enough to melt the surface of rocky bodies and to form shallow lava oceans on them. In case of WASP-12b, this leads to the release of elements such as Mg and Ca, which are expected to surround the system. The predicted Mg and Ca outgassing rates from two Io-sizedWASP-12b Trojans are ?2.2 ? 1027 s-1 and ?2.2 ? 1026 s-1, respectively. Trojan outgassing can lead to the apparent lack of emission in Mg II h&k and Ca II H&K line cores of WASP-12. For HD 189733b, the mechanism is only marginally possible due to the lower temperature. This may be one of the reasons that could not explain the early ingress of HD 189733b observed in the far-UV C II doublet due to absence of carbon within elements outgassed by molten lava. We investigate the long-term stability region of WASP-12b and HD 189733b in case of planar and inclined motion of these satellites and show that unlike the classical exomoons orbiting the planet, Io-sized Trojans can be stable for the whole systems lifetime. © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

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Держатели документа:
Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, Graz, Austria
University of Vienna, Department of Astrophysics, Turkenschanzstrasse 17, Vienna, Austria
IMCCE Observatoire de Paris, Univ. Lille 1, UPMC, 77 Avenue Denfert-Rochereau, Paris, France
Institute of Computational Modelling, Siberian Division of Russian Academy of Sciences, Akademgorodok, ICM SB RAS, Krasnoyarsk, Russian Federation
Siberian Federal University, Svobodnyy pr., 79, Krasnoyarsk, Russian Federation

Доп.точки доступа:
Kislyakova, K. G.; Pilat-Lohinger, E.; Funk, B.; Lammer, H.; Fossati, L.; Eggl, S.; Schwarz, R.; Boudjada, M. Y.; Erkaev, N. V.