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Dynamics of the geomagnetic storm

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Abstract

This paper is intended as a critical review of current ideas concerning the mechanisms responsible for the geomagnetic storm.

The dynamical theory of the geomagnetic storm phenomenon is formulated as a problem in elasticity. The observed variations in the field are the strains produced by particle stresses exerted by gases in interplanetary space, by gases enmeshed in the field, and by the gases in the ionosphere. The stresses exerted by interplanetary gases are principally inward, resulting in the initial phase increase of the horizontal component. The stresses exerted by gases enmeshed in the field are principally outward, resulting in the main phase decrease of the horizontal component. The transient sudden commencement is a hydromagnetic wave phenomenon.

The main phase is most simply explained by the shock heating of the ions to kev energies at 3 – 5 R E during the active phase of the storm. The recovery follows then from charge exchange with the ambient neutral hydrogen. The predicted more rapid recovery at sunspot minimum has been verified observationally.

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Authors and Affiliations

  1. Enrico Fermi Institute for Nuclear Studies and Department of Physics, University of Chicago, 37, Chicago, Illinois

    E. N. Parker

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  1. E. N. Parker
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This work was supported by the National Aeronautics and Space Administration under grant NASA-NsG-96-60.

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Parker, E.N. Dynamics of the geomagnetic storm. Space Sci Rev 1, 62–99 (1962). https://doi.org/10.1007/BF00174636

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  • DOI: https://doi.org/10.1007/BF00174636

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