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

Petrovay, Kristóf and Chaterjee, P. and Choudhuri, A. (2006) Helical Magnetic Fields in Solar Active Regions: Theory vs. Observations. In: 4th Workshop of Young Researchers in Astronomy & Astrophysics. Publications of the Astronomy Department of the Eötvös University (17). ELTE Sokszorosítóüzeme, Budapest, pp. 6-14.

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Abstract

The mean value of the normalized current helicity $\alpha_p=\vc B\cdot(\nabla\times\vc B)/B^2$ 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.

Item Type: Book Section
Additional Information: PADEU Volume 17 4th Workshop of Young Researchers in Astronomy & Astrophysics Edited by E. Forgács-Dajka
Subjects: Q Science / természettudomány > QB Astronomy, Astrophysics / csillagászat, asztrofizika
Depositing User: Emese Kató
Date Deposited: 23 Sep 2024 13:41
Last Modified: 23 Sep 2024 13:45
URI: https://real.mtak.hu/id/eprint/205604

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