Meridional drifts of large-scale solar magnetic fields and meridional circulation

Details Meridional drifts of large-scale solar magnetic fields and meridional circulation Meridional drifts of large-scale solar magnetic fields and meridional circulation

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..851i&link_type=abstract

In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze

Physics

1

Solar Magnetic Fields: Meridional Drifts

Scientific paper

The meridional drifts of local (LF) and large-scale (LSMF) solar magnetic fields has been studied for the time interval 1960-2000. The LSMF meridional drift velocity has been considered as a function of latitude. Two modes have been discovered in the meridional poleward drift of LSMF with the typical equator-to-pole travel times of 16-18 and 2-3 years. It is shown that the variation in the square values of the solar field radial component on the time-latitude diagrams coincides with the equatorward drift of local magnetic fields (LF). A shift by 5-5.5 years is observed in the intensity maxima of the global and local fields. It is shown that the total period of meridional circulation of solar plasma in the convection zone is ~22 years, i.e. is equal to the Hale magnetic cycle.

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