Nonlinear distribution of the sunspot magnetic field during the solar maximum

Details Nonlinear distribution of the sunspot magnetic field during the solar maximum Nonlinear distribution of the sunspot magnetic field during the solar maximum

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003adspr..32.1175r&link_type=abstract

Advances in Space Research, Volume 32, Issue 6, p. 1175-1180.

Computer Science

Scientific paper

Using the standard solar w-dynamo equations we formulate appropriate initial and boundary conditions at the moment when the toroidal component is maximum, so that we obtain the toroidal magnetic field component as a function of the solar latitude. We found a new non-homogeneous distribution for the toroidal component along the latitude (<ΔBθ/Δθ>) given by 7G/degree, 24G/degree and 34G/degree for the respectiives latitudes ranges of 10°-15°, 16°-18° and 19°-25°) and this nonhomogenous decay rate is statistically confirmed through a chi-square analysis of the Mt. Wilson Sunspot data for two solar cycles. Based on this result one can expect the most energetic magnetic eruptive phenomena to be, in average, nonlinearly concentrated at latitudes ranging from 10 to 25 degrees in both hemispheres.

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