Abstract
We calculate helicities of solar active regions based on the idea that poloidal flux lines get wrapped around a toroidal flux tube rising through the convection zone, thereby giving rise to the helicity. We use our solar dynamo model based on the Babcock-Leighton α-effect to study how helicity varies with latitude and time.
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Chatterjee, P. Helicity of solar active regions from a dynamo model. J Astrophys Astron 27, 87–91 (2006). https://doi.org/10.1007/BF02702510
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DOI: https://doi.org/10.1007/BF02702510