The O+ ion flow below the magnetic barrier at Venus

Physics

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Scientific paper

In this study we investigate the properties of O+ ions, more energetic than 10eV, below the magnetosheath boundary of Venus, based on the data collected by the ASPERA 4 plasma analyser flying onboard of the Venus Express Mission. We selected 16 orbits around a special one which was more or less parallel to the Sun-Venus line, from a time interval of +17/-24 days, and a few more half a Venus year before and after. The magnetosheath boundary was identified approximately from the dropout of magnetospheric electrons and the sharp decrease of the proton speed; the entry point correlated well with the location of the magnetic barrier derived by eyes from magnetometer data. Accordingly, the investigation was limited to orbit sections starting near the terminator and ending in the near-tail, the distance from the centre of Venus was always less than 3 RV. The most characteristic structures seen during the various flybys are: a) the inbound and outbound mantle crossings, the inbound being significantly more intense in low energy counts; b) the in- and outbound crossings of the tail boundary, characterized by less intense but higher energy ion beams; c) in cases when geometry permitted, the crossing of the central tail region (current sheet) is is marked by peak low energy ion counts. In several cases the change of the sign of Bx is correlated with high energy O+ 32 ion peaks. These characteristic features together do appear roughly in most cases, the rest are much more variable. The North-South asymmetry of the energy spectra is evident during all the flybys. These results much enhance and refine our previous knowledge concerning the structure of the Venussian tail, because it is based on a much broader data set in a region never explored before.

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