Research examines how solar-wind parameters influence geomagnetic storms, indicating key energetic processes.
An attempt is made to find interplanetary magnetic field and solar-wind parameters which control the development of geomagnetic storms. For this purpose, the interplanetary energy flux is estimated in terms of the Poynting flux (E×B/4π), and its time variations are compared with the rate of energy dissipation in terms of the ring-current particle injection ui(t), Joule dissipation in the ionosphere uj(t) and auroral particle injection up(t) for 15 major geomagnetic storms. A large increase of u(t) is associated with substorm activity. Thus, the energy flux ∈(t) entering the magnetosphere is dissipated through magneto-spheric substorm processes within the magnetosphere, and their accumulated effects can be understood as geomagnetic storm phenomena.
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Perreault et al. (1978) studied this question.
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