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Bulk motion of the magnetosphere

1967; American Geophysical Union; Volume: 72; Issue: 21 Linguagem: Inglês

10.1029/jz072i021p05193

2156-2202

Neil Brice,

Solar and Space Plasma Dynamics

Journal of Geophysical Research (1896-1977)Volume 72, Issue 21 p. 5193-5211 Bulk motion of the magnetosphere Neil M. Brice, Neil M. BriceSearch for more papers by this author Neil M. Brice, Neil M. BriceSearch for more papers by this author First published: 1 November 1967 https://doi.org/10.1029/JZ072i021p05193Citations: 310AboutPDF 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 Fast magnetic field-line merging at the magnetospheric bow and in the tail are examined to determine their implications in regard to the concept of bulk motion of the magnetosphere (convection) and the associated electric field. Upper atmosphere geophysical measurements are surveyed to determine to what extent the available data support this concept. The dawn-dusk asymmetry in energetic particle fluxes, the movement of auroral ionization, ionospheric currents, and the location of the whistler knee (or ‘plasmapause’) are all consistent with this concept, the latter three all giving estimates of the electrostatic potential difference across the magnetosphere in the dawn-dusk meridian of a few tens of kilovolts. A ‘present best estimate’ of the flow pattern in the magnetosphere is derived, based primarily on the diurnal variation in the location of the whistler knee. The convective flow in from the tail appears to be stronger before midnight than after, which is consistent with the location of the maximum nighttime precipitation of energetic electrons. The derived flow is also qualitatively in agreement with that deduced from field-line merging. However, the Axford-Hines types of viscous drag will also give rise to convective flow, and the currently available data do not allow a definitive determination of whether field-line merging or viscous interaction is the principal driving force. References Angerami, J. J., D. L. Carpenter, Whistler studies of the plasmapause in the magnetosphere, 2, Electron density and total tube electron content near the knee in magnetospheric ionization, J. Geophys. Res., 71, 711–725, 1966. Atkinson, G., A theory of polar substorms, J. Geophys. Res., 71, 5157–5164, 1966. Axford, W. I., Viscous interaction between the solar wind and the earth's magnetosphere, Planetary Space Sci., 12, 45–53, 1964. Axford, W. I., C. O. 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J., Radiation trapped in the earth's magnetic field B. M. McCormac, 263–283, D. Reidel Publishing Company, Dordrecht, Holland, 1966. Williams, D. J., G. D. Mead, Nightside magnetosphere configuration as obtained from trapped electrons at 1100 kilometers, J. Geophys. Res., 70, 3017–3029, 1965. Williams, D. J., N. F. Ness, Simultaneous trapped electron and magnetic tail field observations, J. Geophys. Res., 71, 5117–5128, 1966. Citing Literature Volume72, Issue211 November 1967Pages 5193-5211 ReferencesRelatedInformation