Incorporating magnetic buoyancy in solar dynamo models: New results, problems -- and their possible solutions.

Details Incorporating magnetic buoyancy in solar dynamo models: New results, problems -- and their possible solutions. Incorporating magnetic buoyancy in solar dynamo models: New results, problems -- and their possible solutions.

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0134n&link_type=abstract

American Astronomical Society, SPD meeting #31, #01.34

Astronomy and Astrophysics

Astronomy

Scientific paper

There have been traditionally two kinds of approaches to understand the origin of the solar magnetic cycle: the Parker--Steenbeck--Krause--Rädler approach and the Babcock--Leighton approach. It seems at present that the most promising models of the solar dynamo are those which incorporate the best features of both these traditional approaches. One of the uncertainties in these hybrid models (Choudhuri et. al. 1995) lies in the treatment of magnetic buoyancy within a mean field framework, a subject which has rarely been explored in the past (Durney 1997). We study this problem by exploring possible ways of incorporating magnetic buoyancy in a dynamo code -- to simulate the formation and subsequent decay of sunspots and the recycling of fields, with magnetic buoyancy as an important player in the flux-transport process. The results as well as some problems faced by such new generation of dynamo models, will be discussed. References: Durney B. R., 1997, ApJ 486, 1065 Choudhuri A. R., Schussler M., Dikpati M., 1995, A&A 303, L29 Nandi D., Choudhuri A. R., 2000, submitted to ApJ

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