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Theory of the Solar 22-Year Cycle

Published online by Cambridge University Press:  25 April 2016

J. H. Piddington
J. H. Piddington*
Affiliation:
CSIRO Division of Physics, National Standards Laboratory, Sydney
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Extract

If there were no solar magnetic fields, then the most active feature observable on the Sun would be the hydrodynamic convection. There would be no sunspots, flares, prominences, plage, spicules, and no copious emissions of X-rays, energetic particles or radio bursts. These effects are all due to the presence of a changing pattern of magnetic fields which repeats every 22 years. While observations of electromagnetic phenomena are limited to the solar surface and atmosphere, a full understanding of these effects must include a satisfactory theory of the solar cycle and of the fields which evolve beneath the surface as a result of plasma velocity fields.

Type
Invited Papers
Information
Publications of the Astronomical Society of Australia , Volume 2 , Issue 1 , July 1971 , pp. 7 - 10
Copyright
Copyright © Astronomical Society of Australia 1971

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References

1 Babcock, H. W., Astrophys. J., 133, 572 (1961).Google Scholar
2 Kiepenheuer, K. O. in Kuiper, G. P. (ed.), The Sun, University of Chicago Press 1953.Google Scholar
3 de Jager, C., Handbuch Phys., 52, 195 (1959).Google Scholar
4 Cowling, T. G. in Kuiper, G. P. (ed.), The Sun, University of Chicago Press 1953.Google Scholar
5 Parker, E. N., Ann. Rev. Astron. Astrophys., 8, 1 (1970).Google Scholar
6 Parker, E. N., Astrophys. J., 162, 665 (1970).Google Scholar
7 Braginskii, S. I., Soviet Phys. JETP, 20, 726 and 1462 (1965).Google Scholar
8 Leighton, R. B., Astrophys. J., 156, 1 (1969).Google Scholar
9 Piddington, J. H., CSIRO Division Phys. Rep. No. 550 (1971).Google Scholar
10 Bumba, V., Howard, R., Martres, M. J. and Soru-Iscovici, I., Structure and Development of Solar Active Regions, IAU Symp. No. 35, 13 (1968).Google Scholar
11 Piddington, J. H., Cosmic Electrodynamics, Wiley-Interscience, New York 1969.Google Scholar
12 Haurwitz, M. W., Astrophys. J., 151, 351 (1968).CrossRefGoogle Scholar
13 Richardson, R. S. and Schwarzschild, M., Accademia Nationale Lincei Convegno 11, Rome 1952.Google Scholar
14 Allen, C. W., Astrophysical Quantities, 2nd edition, Athlone 1963.Google Scholar