Astronomy and Astrophysics – Astrophysics – Solar and Stellar Astrophysics
Scientific paper
2009-09-24
Astronomy and Astrophysics
Astrophysics
Solar and Stellar Astrophysics
23 pages, 1 figure, Presented at the Fourth UN/ESA/NASA/JAXA Workshop on the International Heliophysical Year and Basic Space
Scientific paper
Two well known turbulent dynamo and MHD oscillation mechanisms are critically examined and fundamental difficulties are presented. Following new ideas on the genesis of the solar cycle and activity phenomena are presented. Inevitability of most likely existence of a combined steady poloidal and toroidal magnetic field structure in the solar interior. Owing to suitable steady poloidal field structure, Alfven wave perturbations of long periods (~ 22 yrs) that excite in the solar core travel first to the poles in both the hemispheres and later reach the equator. While traveling towards the surface, Alfven wave perturbations along the weak poloidal field structure in turn perturb the embedded strong toroidal field structure producing sunspots, especially in the convective envelope, that travel to the surface due to buoyancy along isorotational contours. With realistic density structure of the solar interior, computation of Alfven wave travel times along different field lines of the poloidal field structure (Hiremath and Gokhale 1995) yields almost similar periods (~ 22 yr) explaining the constancy of 22 yr period of the odd degree modes obtained from the Spherical Harmonic Fourier analysis of the surface magnetic field. The observed quasi-periodicities of solar activity indices in the range of 1-5 years are explained due to perturbation of the strong toroidal field structure and, variation of very long period solar cycle and activity phenomena such as the Maunder and grand minima is explained to be due to coupling of long period poloidal and toroidal MHD oscillations.
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