Escape and Energy Relaxation of He and H Atoms and Isotopes in Upper Atmospheres of Terrestrial and Extrasolar Planets

Statistics – Applications

Scientific paper

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[0325] Atmospheric Composition And Structure / Evolution Of The Atmosphere, [0328] Atmospheric Composition And Structure / Exosphere, [0343] Atmospheric Composition And Structure / Planetary Atmospheres

Scientific paper

Accurate parameters of the energy relaxation of He and H atoms in the upper atmosphere of terrestrial and extrasolar planets have been determined. With these parameters, the escape fluxes of He and H atoms and isotopes have been computed for different compositions of the upper atmosphere. The energy relaxation and escape of 3He and 4He isotopes from the Mars atmosphere are analyzed in detail. Rates of energy transfer processes, involving He atoms and major atomic constituents of upper planetary atmospheres (H, He and O), have been computed in ab initio quantum mechanical calculations. Differential, total, and momentum-transfer cross sections, required for a description of the energy-transfer collisions, have been calculated for the broad interval of collision energies from 100K to 10keV and compared with available experimental data. The new database includes information on energy-relaxation parameters of fast He and H atoms in O, H, and He gases, such as the number of collisions required for thermalization, averaged energy loss per collision, and averaged scattering angle as functions of the collision energy. Isotope dependence of the energy-relaxation parameters have been analyzed. To illustrate our results, the new database have been used for a determination of the He escape from the Mars atmosphere and for modeling the precipitation of energetic He atoms produced in interaction of the solar wind alpha particles with the Mars corona. Applications of new data to modeling He and H escape fluxes from atmospheres of the extrasolar planets are discussed.

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