Helical Magnetic Fields in Solar Active Regions: Theory vs. Observations

Details Helical Magnetic Fields in Solar Active Regions: Theory vs. Observations Helical Magnetic Fields in Solar Active Regions: Theory vs. Observations

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006padeu..17....5p&link_type=abstract

In: Proceedings of the 4th Workshop of Young Researchers in Astronomy & Astrophysics; Budapest, Hungary, 11-13 January, 2006; Pu

Astronomy and Astrophysics

Astrophysics

Scientific paper

The mean value of the normalized current helicity α_p=čB\cdot(nabla×čB)/B^2 in solar active regions is on the order of 10^{-8} m^{-1}, negative in the northern hemisphere, positive in the southern hemisphere. Observations indicate that this helicity has a subsurface origin. Possible mechanisms leading to a twist of this amplitude in magnetic flux tubes include the solar dynamo, convective buffeting of rising flux tubes, and the accretion of weak external poloidal flux by a rising toroidal flux tube. After briefly reviewing the observational and theoretical constraints on the origin of helicity, we present a recently developed detailed model for poloidal flux accretion.

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