The Magnetic Structure of the Sun at the Beginning of Solar Cycle 23

Details The Magnetic Structure of the Sun at the Beginning of Solar Cycle 23 The Magnetic Structure of the Sun at the Beginning of Solar Cycle 23

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.9201b&link_type=abstract

American Astronomical Society, 194th AAS Meeting, #92.01; Bulletin of the American Astronomical Society, Vol. 31, p.986

Astronomy and Astrophysics

Astronomy

Scientific paper

The 11-year cycle of solar activity follows Hale's law by reversing the magnetic polarity of leading and following sunspots in bipolar regions during the minima of activity. In the 1996-97 solar minimum, most solar activity emerged in narrow longitudinal zones - `active longitudes' but over a range in latitude. Investigating the distribution of solar magnetic flux, we have found that the Hale sunspot polarity reversal first occurred in these active zones. We have estimated the rotation rates of the magnetic flux in the active zones before and after the polarity reversal. Comparing these rotation rates with the internal rotation inferred by helioseismology, we suggest that both `old' and `new' magnetic fluxes were probably generated in a low-latitude zone near the base of the solar convection zone. The reversal of active region polarity observed in certain longitudes at the beginning of a new solar cycle suggests that the phenomenon of active longitudes may give fundamental information about the mechanism of the solar cycle. The non-random distribution of old-cycle and new-cycle fluxes presents a challenge for dynamo theories, most of which assume a uniform longitudinal distribution of solar magnetic fields. We have used accurate measurements of solar oscillation frequencies from the GONG and SOHO/MDI to infer the latitudinal dependence of the solar structure associated with magnetic fields beneath the surface. The results show significant variations of the aspherical structure of the Sun at the beginning of the new cycle. These variations correlate with the latitudinal distribution of the surface magnetic flux. We discuss possible variations at the base of the convection zone and their relation to the dynamo mechanism.

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