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Plasma-physical aspects of the solar cycle

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Abstract

Mass motions below the photosphere drive the solar cycle which is associated with variations in the magnetic field structure and accompanying phenomena. In addition to semi-empirical models, dynamo theories have been used to explain the solar cycle. The emergence of magnetic field generated by these mechanisms and its expansion into the corona involves many plasma physical processes. Magnetic buoyancy aids the expulsion of magnetic flux. The corona may respond dynamically or by continually adjusting to a quasi-static force-free or pressure-balanced equilibrium. The formation and disruption of current sheets is significant for the overall structure of the coronal magnetic field and the physics of quiescent prominences. The corona has a fine structure consisting of magnetic loops. The structure and stability of these are important as they are one of the underlying elements which make up the corona.

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  1. Department of Plasma Physics, Royal Institute of Technology, S-100 44, Stockholm 70, Sweden

    Michael A. Raadu

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Raadu, M.A. Plasma-physical aspects of the solar cycle. Space Sci Rev 34, 37–45 (1983). https://doi.org/10.1007/BF00221194

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