Hostname: page-component-77c89778f8-cnmwb Total loading time: 0 Render date: 2024-07-23T22:31:38.653Z Has data issue: false hasContentIssue false
  • English
  • Français

A Topological Model of the Solar Magnetic Field Reversals

Published online by Cambridge University Press:  12 April 2016

E.E. Benevolenskaya
E.E. Benevolenskaya*
Affiliation:
Pulkovo Astronomical Observatory, 196140, Leningrad, USSR

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The phenomenon of a three-fold reversal of the solar polar magnetic field in both hemispheres has not been observed during the last 115 years. Such three-fold reversals took place in the southern hemisphere alone in the even cycles Nos 12 (1885.8), 14 (1908.4) and in the northern hemisphere alone in solar cycles Nos 16 (1928.5), 18 (1949.0), 20 (1970.6). The single reversal took place in the odd cycles, the only exception is the solar cycle No 19 (Fig. 1).

There are periods of 1.7-2.5 years in the variation of background magnetic fields (Makarov et al., 1985). It determines the quasi-period of the high-frequency component and corresponds to a time interval between the zones of alternating polarity of the magnetic field. This enables us to show topologically that single and three-fold polarity reversals of the solar magnetic fields can result from interaction of two types of magnetic fields: a low-frequency component with period of the order of 20 years and a high frequency component with period of order of 1.7-2.5 years (Benevolenskaya and Makarov, 1990).

Type
Part III Solar magnetism and large-scale flows
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 234 - 236
Copyright
Copyright © Springer-Verlag 1991

References

Benevolenskaya, E.E. and Makarov, V.I.: 1990, Soln. Dann. No 5, 75 Google Scholar
Hoyng, P.: 1990 in Solar Photosphere: Structure, Convection and Magnete Fields, ed. Stenflo, O.J., IAU Symp. No 138, p. 359 Google Scholar
Kleeorin, N.I. and Ruzmaikin, A.A: 1988, Preprint IZMIRAN, No 7(833), p. 3 Google Scholar
Makarov, V.I., Tavastsherna, K.S. and Petrova, N.S.: 1985, Soln. Dann. No 6, 69 Google Scholar
Parker, E.N.: 1979, Cosmical Magnetic Fields, Oxford University Press.Google Scholar
Wang, J.W., Nash, A.G. and Sheeley, N.R. Jr.: 1989, Astrophys. J. 347, 529 Google Scholar