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[Text] / K. G. Lichtenegger [et al.] // J. Geophys. Res-Space Phys. - 2016. - Vol. 121, Is. 5. - P4718-4732, DOI 10.1002/2015JA022226. - Cited References:60. - H.I.M. Lichtenegger acknowledges support from the FWF project P24247-N16, and N.V. Erkaev, M. Gudel, K.G. Kislyakova, C.P. Johnstone, and H. Lammer acknowledge the support by the FWF NFN project S11601-N16 "Pathways to Habitability: From Disks to Active Stars, Planets and Life" and the related FWF NFN subprojects, S11604-N16 "Radiation & Wind Evolution from T Tauri Phase to ZAMS and Beyond", and S11607-N16 "Particle/Radiative Interactions with Upper Atmospheres of Planetary Bodies Under Extreme Stellar Conditions." N.V. Erkaev, H. Lammer, and P. Odert acknowledges also support from the FWF project P27256-N27. N.V. Erkaev was also supported by the RFBR grant 15-05-00879-a. This research was conducted using resources provided by the Swedish National Infrastructure for Computing (SNIC) at the High Performance Computing Center North (HPC2N), Umea University, Sweden. The software used in this work was in part developed by the DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago. The data can be provided by H. I. M. Lichtenegger (herbert.lichtenegger@oeaw.ac.at) and K.G. Kislyakova (kristina.kislyakova@oeaw.ac.at). . - ISSN 2169-9380. - ISSN 2169-9402РУБ Astronomy & Astrophysics

Аннотация: We present a study on the influence of the upper atmosphere hydrodynamic escape of hydrogen, driven by the solar soft X-ray and extreme ultraviolet radiation (XUV), on an expected outgassed steam atmosphere of early Venus. By assuming that the young Sun was either a weak or moderately active young G star, we estimated the water loss from a hydrogen dominated thermosphere due to the absorption of the solar XUV flux and the precipitation of solar wind produced energetic hydrogen atoms (ENAs). The production of ENAs and their interaction with the hydrodynamic extended upper atmosphere, including collision-related feedback processes, have been calculated by means of Monte Carlo models. ENAs that collide in the upper atmosphere deposit their energy and heat the surrounding atmosphere mainly above the main XUV energy deposition layer. It is shown that precipitating ENAs modify the thermal structure of the upper atmosphere, but the enhancement of the thermal escape rates caused by these energetic hydrogen atoms is negligible. Our results also indicate that the majority of oxygen arising from dissociated H2O molecules is left behind during the first 100Myr. It is thus suggested that the main part of the remaining oxygen has been absorbed by crustal oxidation.

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Держатели документа:
Austrian Acad Sci, Space Res Inst, Graz, Austria.
SB RAS, Inst Computat Modelling, Krasnoyarsk, Russia.
Siberian Fed Univ, Polytech Inst, Krasnoyarsk, Russia.
Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
Univ Vienna, Dept Astrophys, Vienna, Austria.
Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
Swedish Inst Space Phys, Kiruna, Sweden.

Доп.точки доступа:
Lichtenegger, H. I. M.; Kislyakova, K. G.; Odert, N. V.; Erkaev, N. V.; Lammer, H.; Groller, C. P.; Johnstone, C. P.; Elkins-Tanton, L.; Tu, M.; Gudel, M.; Holmstrom, M.; FWF [P24247-N16, P27256-N27]; FWF NFN [S11601-N16, S11604-N16, S11607-N16]; RFBR [15-05-00879-a]