The post-terminator ionosphere of Venus

• Published in: Icarus (New York, N.Y. 1962) N.Y. 1962), 2011-12, Vol.216 (2), p.625-639
• Main Author: Fox, Jane L.
• Format: Article
• Language: English
• Subjects: Astronomy; Atmospheres, Chemistry; Atmospheres, Composition; Density; Earth, ocean, space; Exact sciences and technology; Fluxes; Ionosphere; Ionospheres; Mathematical models; Morphology; Solar activity; Solar system; Thermosphere; Venus; Venus, Atmosphere
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2011.09.020

► We study photoionization and downward ion fluxes in the nightside Venus ionosphere. ► We find that the ionosphere is sunlit to 95°SZA or slightly more. ► We find that the downward ion flux over the 90–125° range is 1.2E8cm−2s−1. ► We find that the nightside ne peaks are systematically higher than the RO profiles. ► We suggest that the VTS3 neutral densities are too large over the entire nightside. We have modeled the near and post-terminator thermosphere/ionosphere of Venus with a view toward understanding the relative importance of EUV solar fluxes and downward fluxes of atomic ions transported from the dayside in producing the mean ionosphere. We have constructed one-dimensional thermosphere/ionosphere models for high solar activity for seven solar zenith angles (SZAs) in the dusk sector: 90°, 95°, 100°, 105°, 110°, 115° and 125°. For the first 4SZAs, we determine the optical depths for solar fluxes from 3Å to 1900Å by integrating the neutral densities numerically along the slant path through the atmosphere. For SZAs of 90°, 95°, and 100°, we first model the ionospheres produced by absorption of the solar fluxes alone; for 95°, 100°, and 105°SZAs, we then model the ion density profiles that result from both the solar source and from imposing downward fluxes of atomic ions, including O+, Ar+, C+, N+, H+, and He+, at the top of the ionospheric model in the ratios determined for the upward fluxes in a previous study of the morphology of the dayside (60°SZA) Venus ionosphere. For SZAs of 110°, 115° and 125°, which are characterized by shadow heights above about 300km, the models include only downward fluxes of ions. The magnitudes of the downward ion fluxes are constrained by the requirement that the model O+ peak density be equal to the average O+ peak density for each SZA bin as measured by the Pioneer Venus Orbiter Ion Mass Spectrometer. We find that the 90° and 95°SZA model ionospheres are robust for the solar source alone, but the O+ peak density in the “solar-only” 95°SZA model is somewhat smaller than the average value indicated by the data. A small downward flux of ions is therefore required to reproduce the measured average peak density of O+. We find that, on the nightside, the major ion density peaks do not occur at the altitudes of peak production, and diffusion plays a substantial role in determining the ion density profiles. The average downward atomic ion flux for the SZA range of 90–125° is determined to be about 1.2×108cm−2s−1.