Solar cycle variations of electron density and temperature in the Venusian nightside ionosphere

Details Solar cycle variations of electron density and temperature in the Venusian nightside ionosphere Solar cycle variations of electron density and temperature in the Venusian nightside ionosphere

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993georl..20.2719t&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 20, no. 23, p. 2719-2722

Physics

11

Electron Density (Concentration), Electron Energy, Night, Planetary Ionospheres, Solar Cycles, Solar Planetary Interactions, Venus (Planet), Conductive Heat Transfer, Depletion, Electron Probes, Ions, Mathematical Models, Pioneer Venus 1 Spacecraft

Scientific paper

The return of periapsis to low altitudes during the Summer and Fall of 1992 provided a unique opportunity for the Pioneer Venus Orbiter (PVO) to make in situ measurements in the Venusian ionosphere at much lower levels of solar activity (F10.7 approx. equals 120) than existed when periapsis was at low altitudes in 1979 and 1980 (F10.7 approx. equals 220). We present the observations of electron density (Ne) and temperature (Te) made by the Orbiter Electron Temperature Probe (OETP) during the Entry Period. Empirical models of the Ne and Te height variations are presented and compared with similar models based on OETP measurements made at solar maximum. The median Ne at the ionospheric peak (approx. 140 km) was essentially unchanged from its solar maximum value, but the ionosphere was increasingly depleted at higher altitudes, reaching a factor of 7 lower densities at 200 km. Te was lower by almost a factor of 2 at 140 km but was rather significantly enhanced at higher altitudes; exceeding its solar maximum values by a factor of 1.3 at 200 km and a factor of 2 at 500 km. In general these results support the earlier conclusions that the nightside upper ionosphere is depleted at lower levels of solar activity by a reduction of the nightward ion flow. The lack of Ne variation near the peak (between solar maximum and entry) suggests that nightward ion transport does not play as large a role in the peak formation as does local ion production by energetic particles. The decrease does local ion production by energetic particles. The decrease in Te at low altitudes suggests that the low densities of the upper ionosphere at the time of PVO entry could no longer support the conduction of heat from the dayside ionosphere, thus allowing the lower nightside ionosphere to cool by collisions with ions and neutrals, and by heat conduction to the cooler regions below.

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