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Valentina Zharkova   Submitted: 2008-02-07 07:59

The observed phase relations between the weak background solar magnetic (poloidal) field and strong magnetic field assocciated wtih sunspots (toroidal field) measured at different latitudes are presented. For measurements of the solar magnetic field (SMF) the low-resolution images obtained from Wilcox Solar Observatory (WSO) are used while sunspot magnetic field was taken from the Solar Feature Catalogues utilizing the SOHO/MDI fulldisk magnetograms. The quasi-3D latitudinal distributions of sunspot areas and magnetic elds obtained for 30 latitudinal bands (15 in the northern and 15 in the southern hemispheres) within the whole mu-hemispheres in longitudes are correlated with those of the background SMF. The sunspot areas in all latitudinal zones (averaged with a sliding one-year filter) reveal a strong positive correlation with the absolute SMF in the same zone appearing rst with a zero timelag and repeating with a two  three year time lag through the whole period of observations. The residuals of the sunspot areas averaged by one year and those by four years are also shown to have a well defined periodic structure visible in every two - three years close to pi/4 with the maxima occurring at -40 and +40 degrees in latitude and the drifts during this period either towards the Equator or the Poles depending on the latitude of sunspot occurrence. This phase relation between poloidal and toroidal field throughout the whole cycle is discussed in association with both the symmetric and asymmetric components of the background SMF and relevant predictions by the solar dynamo models.

Authors: Zharkov S.I., Gavryuseva,E. and Zharkova V.V
Projects: SoHO-MDI

Publication Status: Solar Physics, in press
Last Modified: 2008-02-07 09:22
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