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Solar Wind Interaction with Venus, Mars and Comets

Published online by Cambridge University Press:  25 April 2016

M.K. Wallis

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To model and quantify the comet-like interactions with the atmosphere of Venus the extent and time-variability of the suprathermal exospheric coronas need to be established. An extensive suprathermal O corona hypothesized to arise via dissociative recombination of the dominant ion was confirmed by the Orbiter’s UV spectrometer. Uncertainties remain, firstly because the O-corona’s extension beyond the observed limit of 1500 km altitude depends on the poorly-known partition between dissociation channels, secondly because the ionosphere varies substantially with solar UV inputs, and thirdly because the ionosphere and therefore O-corona decrease strongly from dayside to nightside (Kliore et al., Adv. Space Res. 5(11), 1985).

Type
Research Article
Information
Transactions of the International Astronomical Union , Volume 20 , Issue 1 , 1988 , pp. 683 - 689
Copyright
Copyright © Kluwer 1988 

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