Magnetospheric convection

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Abstract
Magnetospheric convection, which implies the existence of large‐scale electric fields, appears to be the dominant process for the acceleration and injection of moderately energetic plasma into the magnetosphere. The aurora, the radiation belts, and the ‘thermal’ plasma beyond the plasmapause are directly controlled by the convection induced by the solar wind. The existence of the plasmapause and its variations with time can be understood in terms of convection, and, even within the plasmapause, the radiation belts and the ionospheric plasma are strongly affected by tidally induced convection and the more random convection associated with DP1 and DP2 geomagnetic activity. The basic features of convection are discussed briefly in this review. Direct and indirect observations that provide evidence for the existence of convection are described, and the expected nature of the solar‐wind‐induced convection in the outer magnetosphere is discussed at some length. A fairly complete bibliography concerning the theory of magnetospheric convection is provided in the references.

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