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

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dc.creatorPetrovay, K.
dc.creatorChaterjee, P.
dc.creatorChoudhuri, A.
dc.date2007-02-02
dc.date.accessioned2026-07-07T10:21:42Z
dc.date.available2026-07-07T10:21:42Z
dc.descriptionThe mean value of the normalized current helicity in solar active regions is on the order of 1e-8 1/m, 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.
dc.description10 pages, 5 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0702073
dc.identifierhttp://arxiv.org/abs/astro-ph/0702073
dc.identifierPubl.Astron.Dep.EotvosUniv.17:5-14,2006
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175263
dc.subjectAstrophysics
dc.titleHelical Magnetic Fields in Solar Active Regions: Theory vs. Observations
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