Electron Observations in the Solar Wind and Magnetosheath at Venus

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Scientific paper

We have analyzed electron data recorded by the retarding potential analyzer (RPA) flown on the Pioneer Venus Orbiter (PVO). In order to do so, we first developed a routine to evaluate the transmission function of the instrument based on the size, width, and spacing of the grid stack in front of the collector. We have used the transmission function in a least squares fitting approach to derive electron parameters in the solar wind and magnetosheath near Venus. Within the solar wind, we have assumed that the distribution function describing the electron population is dominated by a single Maxwellian component. Such an assumption is supported by other measurements. In the magnetosheath, we have compared the use of a flat-topped distribution to the use of a single Maxwellian distribution. The total density determined for the two distributions did not differ more than the expected error for either one separately. By using the data from several hundred orbits, we have developed a picture of the average electron density and temperature structure within the magnetosheath of the planet (between the bow shock and ionopause). Finally, we have used results to calculate the mass addition and ionization rates due to energetic electron impacts on planetary neutrals. Our calculated rate compares favorably to the rate determined based on inputs from the gas dynamic model carried out by other researchers. Our work thus supports the hypothesis that impact electron ionization is a significant source of mass addition to the solar wind flow around Venus and may therefore, along with photoionization, be responsible for lifting the bow shock above the terminator.

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