On the thermal loss of a planetary atmosphere due to irradiation by the solar EUV during earlier and present epochs

Details On the thermal loss of a planetary atmosphere due to irradiation by the solar EUV during earlier and present epochs On the thermal loss of a planetary atmosphere due to irradiation by the solar EUV during earlier and present epochs

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..849k&link_type=abstract

European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a

Computer Science

Scientific paper

Abstract. Since early 1980's a number of idealized hydrodynamic models have been developed to study thermal atmospheric escape from terrestrial planets due to extreme solar EUV-heating which was expected during the fist billion years after the Sun arrived to the Zero- Age-Main-Sequence. Later on such a type of "hydro-escape" models have been extrapolated to include also low mass outer solar system planets like Titan and Pluto irradiated by the present time solar EUV flux. From all these models Parker-type supersonic solutions have been obtained with a transonic point typically located at a distance of about 10 planetary radii or more from the planets. We have examined critically these idealized hydrodynamic models and found that the assumptions on which they are based are incompatible with the obtained supersonic solutions. As a result the thermal loss rates in the "hydro-escape" models seem to be grossly overestimated, temperature and density altitude profiles substantially deformed. An approximate method to solve this hydrodynamic modelling problem which is based on a combination of the hydrodynamic and kinetic approaches for estimating atmospheric loss from a planetary atmosphere exposed to high solar EUV radiation is suggested and analysed and its application to a specific planet is discussed.

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