Solar Wind Stimulation of the Magnetosphere
The manner in which the solar wind stimulates geomagnetic activity has been a subject of interest since spacecraft measurements of the solar wind and interplanetary magnetic field became available. It was demonstrated with Mariner 2 measurements that a rough relationship exists between solar wind bulk speed and geomagnetic activity (Snyder et al., 1963). The average size of the magnetosphere is less at times of high Kp, suggesting that the solar wind pressure is greater then (Gosling et al., 1967). Sudden commencements and impulses in the geomagnetic field are produced by interplanetary shocks and discontinuities as reported by a number of groups (e.g., Gosling et al., 1968). Increases in the solar wind proton density and α-particle abundance which occur following interplanetary shocks, and at about the time of the main phase development of geomagnetic storms, have also been reported (e.g., Bame et al., 1968; Hirshberg et al., 1970). The importance of a southward directed magnetosheath magnetic field for the production of disturbances has been reported by Fairfield and Cahill(1966). Numerous other studies have been published but space precludes a discussion of them here.
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- Fairfield, D. H.: 1968, Space Research VIII, p. 107.Google Scholar