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Title:
Origin and loss of nebula-captured hydrogen envelopes from `sub'- to `super-Earths' in the habitable zone of Sun-like stars
Authors:
Lammer, H.; Stökl, A.; Erkaev, N. V.; Dorfi, E. A.; Odert, P.; Güdel, M.; Kulikov, Yu. N.; Kislyakova, K. G.; Leitzinger, M.
Affiliation:
AA(Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, A-8042 Graz, Austria ), AB(Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, A-1180 Vienna, Austria), AC(Institute for Computational Modelling, Russian Academy of Sciences, Krasnoyarsk 660036, Russian Federation; Siberian Federal University, Krasnoyarsk 660036, Russian Federation), AD(Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, A-1180 Vienna, Austria), AE(Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, A-8042 Graz, Austria; Institute of Physics, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria), AF(Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, A-1180 Vienna, Austria), AG(Polar Geophysical Institute, Russian Academy of Sciences, Khalturina Str. 15, Murmansk 183010, Russian Federation), AH(Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, A-8042 Graz, Austria), AI(Institute of Physics, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 439, Issue 4, p.3225-3238 (MNRAS Homepage)
Publication Date:
04/2014
Origin:
OUP
Astronomy Keywords:
hydrodynamics, planets and satellites: atmospheres, planets and satellites: physical evolution, ultraviolet: planetary systems
Abstract Copyright:
2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stu085
Bibliographic Code:
2014MNRAS.439.3225L

Abstract

We investigate the origin and loss of captured hydrogen envelopes from protoplanets having masses in a range between `sub-Earth'-like bodies of 0.1 M and `super-Earths' with 5 M in the habitable zone at 1 au of a Sun-like G star, assuming that their rocky cores had formed before the nebula gas dissipated. We model the gravitational attraction and accumulation of nebula gas around a planet's core as a function of protoplanetary luminosity during accretion and calculate the resulting surface temperature by solving the hydrostatic structure equations for the protoplanetary nebula. Depending on nebular properties, such as the dust grain depletion factor, planetesimal accretion rates, and resulting luminosities, for planetary bodies of 0.1-1 M we obtain hydrogen envelopes with masses between ˜2.5 × 1019 and 1.5 × 1026 g. For `super-Earths' with masses between 2 and 5 M more massive hydrogen envelopes within the mass range of ˜7.5 × 1023-1.5 × 1028 g can be captured from the nebula. For studying the escape of these accumulated hydrogen-dominated protoatmospheres, we apply a hydrodynamic upper atmosphere model and calculate the loss rates due to the heating by the high soft-X-ray and extreme ultraviolet (XUV) flux of the young Sun/star. The results of our study indicate that under most nebula conditions `sub-Earth' and Earth-mass planets can lose their captured hydrogen envelopes by thermal escape during the first ˜100 Myr after the disc dissipated. However, if a nebula has a low dust depletion factor or low accretion rates resulting in low protoplanetary luminosities, it is possible that even protoplanets with Earth-mass cores may keep their hydrogen envelopes during their whole lifetime. In contrast to lower mass protoplanets, more massive `super-Earths', which can accumulate a huge amount of nebula gas, lose only tiny fractions of their primordial hydrogen envelopes. Our results agree with the fact that Venus, Earth, and Mars are not surrounded by dense hydrogen envelopes, as well as with the recent discoveries of low density `super-Earths' that most likely could not get rid of their dense protoatmospheres.
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