The magnetosphere under the radial interplanetary magnetic field: A numerical study. Issue 12 (17th December 2013)

• Record Type: Journal Article
• Authors: Tang, B. B.; Wang, C.; Li, W. Y.
• Is Part Of: Journal of geophysical research. Volume 118:Issue 12(2013:Dec.)
• Page Start: 7674
• Page End: 7682
• Publication Date: 2013-12-17
• Subjects: Magnetospheric physics -- Periodicals; Space environment -- Periodicals; Cosmic physics -- Periodicals; Planets -- Atmospheres -- Periodicals; Heliosphere (Astrophysics) -- Periodicals; Geophysics -- Periodicals; 523.01
• DOI: 10.1002/2013JA019155
• Languages: English
• ISSNs: 2169-9380

Abstract

<abstract abstract-type="main" id="jgra50731-abs-0001"> <title> <x xml:space="preserve">Abstract</x> </title> <p id="jgra50731-para-0001">[1] We investigate the magnetosphere under radial interplanetary magnetic fields (IMF) by using global magnetohydrodynamic simulations. The magnetosphere‐ionosphere system falls into an unexpected state under this specific IMF orientation when the solar wind electric field vanishes. The most important features that characterize this state include (1) magnetic reconnections can still occur, which take place at the equatorward of the cusp in one hemisphere, the tailward of the cusp in the other hemisphere, and also in the plasma sheet; (2) significant north‐south asymmetry exists in both magnetosphere and ionosphere; (3) the polar ionosphere mainly presents a weak two‐cell convection pattern, with the polar cap potential valued at ∼30 kV; (4) the whole magnetosphere‐ionosphere system stays in a very quiet state, and the <italic>AL</italic> index does not exceed −70 nT; and (5) the Kelvin‐Helmholtz instability can still be excited at both flanks of the magnetosphere. These results imply the controlling role of the IMF direction between the solar wind and magnetosphere interactions and improve our understanding of the solar wind‐magnetosphere‐ionosphere system.</p> </abstract>