Non-thermal hydrogen in the Venus exosphere - The ionospheric source and the hydrogen budget

Details Non-thermal hydrogen in the Venus exosphere - The ionospheric source and the hydrogen budget Non-thermal hydrogen in the Venus exosphere - The ionospheric source and the hydrogen budget

Nov 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978p%26ss...26.1063k&link_type=abstract

(International Association of Geomagnetism and Aeronomy, General Assembly, 3rd, Seattle, Wash., Aug. 22-Sept. 3, 1977.) Planetar

Astronomy and Astrophysics

Astronomy

9

Atmospheric Composition, Exosphere, Hydrogen, Planetary Ionospheres, Venus Atmosphere, Astronomical Models, Atmospheric Models, Charge Exchange, Hydrogen Atoms, Lower Ionosphere, Solar Wind, Spaceborne Astronomy, Upper Atmosphere, Upper Ionosphere

Scientific paper

A nonthermal, or 'hot', Venus corona of H atoms has been observed by Mariners 5 and 10 and Venera 9. Of the sources investigated, reaction of H2 with ionospheric O(+) is still the strongest. It can explain the smaller densities but falls somewhat short of the largest (from Mariner 5). The subsequent recombination of OH(+), supplemented by solar-wind processes, may give an escape flux of 10 million atoms per sq cm/s. The low density of thermal H atoms on the day side has previously been attributed to either a large eddy diffusion coefficient or an escape flux tenfold greater than this. An alternative mechanism, suggested by Hartle and Mayr (1977) is supported: the hydrogen is swept to the night side by strong thermospheric winds. This process is analogous to the 'Johnson pump' for the terrestrial winter helium bulge. Large nightside bulges of H and H2 are predicted; the night/day density ratio is estimated to be as large as 100 for each.

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