Thermospheric X-Ray and Euv Heating by the Young Sun on Early Venus and Mars

Details Thermospheric X-Ray and Euv Heating by the Young Sun on Early Venus and Mars Thermospheric X-Ray and Euv Heating by the Young Sun on Early Venus and Mars

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006ssrv..122..189l&link_type=abstract

Space Science Reviews, Volume 122, Issue 1-4, pp. 189-196

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6

Thermospheric Heating, Exospheres, Water Loss, Young Sun, Venus, Mars

Scientific paper

In view of the low H2O abundance in the present Venusian and Martian atmospheres several observations by spacecraft and studies suggest that both planets should have lost most of their water over the early active period of the young Sun. During the first Gyr after the Sun arrived at the Zero- Age-Main-Sequence high X-ray and EUV fluxes between 10 and 100 times that of the present Sun were responsible for much higher temperatures in the thermosphere-exosphere environments on both planets. By applying a diffusive-gravitational equilibrium and thermal balance model for investigating radiation impact on the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by CO2 IR emission in the 15μm band we found expanded thermospheres with exobase levels between about 200 km (present) and 2000 km (4.5 Gyr ago). The higher temperatures in the upper atmospheres of both planets could reach “blow-off” conditions for H atoms even at high CO2 mixing ratios of 96%. Lower CO2/N2 mixing ratio or higher contents of H2O vapor in the early atmospheres could have had a dramatic impact from the loss of atmosphere and water on both planets. The duration of this phase of high thermal loss rates essentially depended on the mixing ratios of CO2, N2, and H2O in the early atmospheres and could have lasted between about 150 and several hundred Myr.

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