High-latitude plasma transport: The polar wind
1969; American Geophysical Union; Volume: 74; Issue: 26 Linguagem: Inglês
10.1029/ja074i026p06317
ISSN2156-2202
Autores Tópico(s)Astro and Planetary Science
ResumoJournal of Geophysical Research (1896-1977)Volume 74, Issue 26 p. 6317-6332 High-latitude plasma transport: The polar wind Peter M. Banks, Peter M. BanksSearch for more papers by this authorThomas E. Holzer, Thomas E. HolzerSearch for more papers by this author Peter M. Banks, Peter M. BanksSearch for more papers by this authorThomas E. Holzer, Thomas E. HolzerSearch for more papers by this author First published: 1 December 1969 https://doi.org/10.1029/JA074i026p06317Citations: 254AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onEmailFacebookTwitterLinkedInRedditWechat Abstract Within the polar regions of the earth, magnetic field lines do not form closed loops but are open to the tail of the magnetosphere and interplanetary conditions. Owing to the low plasma pressure in the tail, outward transport of ionospheric plasma takes place with H+ and He+ reaching supersonic speeds at 2000–5000 km altitude. The loss of light ions from the topside polar ionosphere leaves O+ as a dominant ion to great altitudes and results in very low ambient electron concentrations. Typical escape fluxes calculated for H+ and He+ are in the ranges 2–7 × 108 cm−2 sec−1 and 2–4 × 106 cm−2 sec−1, respectively. When magnetospheric convection is taken into account, the escape of ionospheric plasma can lead to the formation of a sharp latitudinal density gradient (the plasmapause) at the boundary between corotating and convecting magnetic field lines. 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