Large-scale structure of solar magnetic cyclicity

Details Large-scale structure of solar magnetic cyclicity Large-scale structure of solar magnetic cyclicity

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993azh....70..543m&link_type=abstract

Astronomicheskij Zhurnal (ISSN 0004-6299), vol. 70, no. 3, p. 543-555.

Astronomy and Astrophysics

Astronomy

5

Chromosphere, Solar Activity, Solar Cycles, Solar Magnetic Field, Magnetic Flux, Solar Corona

Scientific paper

Energy parameter calculations via spherical functions are used to determine the causal relationships between structures of the large-scale solar magnetic field over the last eight cycles on the basis of synoptic chromosphere formation charts of the Meudon Observatory (France). It is shown that the first large-scale magnetic field sector mode is the 'source' of the solar activity. This magnetic field mode is associated with correlations with the poloidal magnetic field energy of the next maxima and with the level of sunspot formation activity of the subsequent maxima. The cycle amplitude formation process modeled from the found relationships has stochastic characteristics. The level of the next, 23rd, solar cycle is predicted to be high (higher than the level of cycle 19, and that of cycle 24 is expected to be low (at the level of cycle 16).

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