Thermal and non-thermal escape of hydrogen and oxygen at Venus

Details Thermal and non-thermal escape of hydrogen and oxygen at Venus Thermal and non-thermal escape of hydrogen and oxygen at Venus

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....12140l&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #12140

Physics

Scientific paper

The evolution of the Venusian atmosphere is influenced by thermal escape processes of H and H2 as well as non-thermal loss processes of H+, H2+, O, O+, CO2 and O2+ caused by the interaction of the solar wind with the planetary atmosphere and possible chemical weathering with the surface. We use a gas dynamic test particle model which involves the motion in the interplanetary electric and magnetic field for the estimation of the loss rates of both pick up ions as well as energetic neutral atoms (ENAs). We also include photochemically produced very low energetic hydrogen and oxygen atoms (VLENAs) whose escape rates are determined by means of Monte Carlo particle simulations. Further, we discuss the loss rates due to atmospheric sputtering and ionospheric bubbles triggered by Kelvin Helmholtz instabilities. By assuming that water vapour is the major source of hydrogen in the Venusian atmosphere we study whether the ratio between H:O escape to space is 2:1; any higher ratio would imply additional planetary sinks for oxygen. Moreover, our results will be of relevance in view of the upcoming VEX-MAG and ASPERA-4 observations aboard Venus Express.

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