Computer Science
Scientific paper
Sep 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989p%26ss...37.1063b&link_type=abstract
Planetary and Space Science (ISSN 0032-0663), vol. 37, Sept. 1989, p. 1063-1077.
Computer Science
1
Exosphere, Pressure Effects, Radiation Pressure, Solar Radiation, Venus Atmosphere, Atmospheric Models, Energetic Particles, Gas Ionization, Hydrogen Atoms, Lyman Alpha Radiation
Scientific paper
The existence of a 'hot' population of hydrogen atoms in the Venus exosphere is well known. In the outer coronal region where it is dominant, r greater than about 2.0 R(V) (Venus radii), hydrogen atoms are also subject to a relatively strong radiation pressure exerted by resonant scattering of solar Lyman-alpha photons. Collisionless models illustrating the consequent structure are discussed, with the nonthermal population mimicked by a dual Maxwellian exobase kinetic distribution. In these models, a considerable fraction of the 'hot' atoms outside 2.0 R(V) belongs to the quasi-satellite component, this fraction exceeding 1/2 for r values between about 4.0 and 10.0 R(V). Solar ionization of bound atoms occurs mainly outside the ionopause, yielding a partial escape flux greater than about 2,000,000/sq cm per sec over the dayside exobase for assumed solar conditions. The inclusion of a cold exobase prescribed by Pioneer Venus observations has little influence on the outer region (in particular, the quasi-satellite component is unaltered) except that the transition to 'hot' kinetic character occurs closer to the exobase on the nightside due to the colder main exobase temperatures there.
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