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dc.contributor.authorOdera, T. J.
dc.date.accessioned2016-08-04T14:29:44Z
dc.date.available2016-08-04T14:29:44Z
dc.date.issued1986-02
dc.identifier.citationAmerican Geophysical Union Volume 24, Issue 1 February 1986 Pages 55–74en_US
dc.identifier.issn8755-1209
dc.identifier.urihttp://ir-library.ku.ac.ke/handle/123456789/14865
dc.descriptionResearch articleen_US
dc.description.abstractAbstract Studies of the solar wind controlled Pc 3, 4 pulsations by early and recent researchers are highlighted. The review focuses on the recent observations, which cover the time during the International Magnetospheric Study (IMS). Results from early and recent observations agree on one point, that is, that the Pc 3, 4 pulsations are influenced by three main solar wind parameters, namely, the solar wind velocity Vsw, the IMF orientation θxB, and magnitude B. The results can be interpreted, preferably, in terms of an external origin for Pc 3, 4 pulsations. This implies, essentially, the signal model, which means that the pulsations originate in the upstream waves (in the interplanetary medium) and are transported by convection to the magnetopause, where they couple to oscillations of the magnetospheric field lines.en_US
dc.language.isoenen_US
dc.publisherReviews of Geophysicsen_US
dc.titleSolar wind controlled pulsations: A reviewen_US
dc.typeArticleen_US


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