Studies of the chemistry of the nightside ionosphere of Venus

Details Studies of the chemistry of the nightside ionosphere of Venus Studies of the chemistry of the nightside ionosphere of Venus

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991suny.rept.....f&link_type=abstract

Final Report, 1 Jul. 1988 - 30 Nov. 1990 State Univ. of New York, Stony Brook. Inst. for Terrestrial and Planetary Atmospheres.

Mathematics

Atmospheric Chemistry, Atmospheric Models, Ion Motion, Ionospheric Ion Density, Mathematical Models, Planetary Ionospheres, Venus Atmosphere, Carbon Monoxide, Ionization Potentials, Night Sky, Nightglow, Nitrogen Ions, Oxygen Ions, Pioneer Venus Spacecraft, Transport Theory, Venus (Planet)

Scientific paper

A combination of numerical modeling and analysis of the Pioneer Venus UADS data base is studied, specifically data from the orbiter ion mass spectrometer (OIMS), orbiter neutral mass spectrometer (ONMS), and orbiter electron temperature probe (OETP). A one dimensional model of the Venus nightside ionosphere was set up in which downward fluxes of atomic ions are introduced at the upper boundary to simulate transport of ions from the dayside. The model shows that the densities of mass-28 ions, CO(+) + N(2+), resulting from an influx of atomic ions from the dayside are quite small, due to the high ionization potentials of CO and N2 that make chemical production difficult. A look at the data reveals that the actual densities of mass-28 ions are quite variable, from values near 10 to more than 104 cm-3. The excess mass-28 ions are assumed to be produced by electron precipitation and that the presence of high densities of mass-28 ions is a signature of auroral precipitation. A discussion of the atomic oxygen green line in the nightglow of Venus, which is produced mainly by dissociative recombination of O(2+), is presented. Original calculations of production rates of excited states for models based on Pioneer Venus data are also presented.

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