Physics
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.0405m&link_type=abstract
American Astronomical Society, SPD meeting #40, #4.05; Bulletin of the American Astronomical Society, Vol. 41, p.810
Physics
Scientific paper
The best tool we have for understanding the origin of solar magnetic variability is the kinematic dynamo model. During the last decade this type of models have seen a continuous evolution and have become increasingly successful at reproducing solar cycle characteristics. However, some of the key ingredients used in dynamo models remain poorly constrained which allows one to obtain solar-like solutions by "tuning" the input parameters. Here we present out efforts to better constrain two of the most important ingredients of solar dynamo models:: The internal velocity field (meridional flow and differential rotation) and the turbulent diffusivity. To accomplish this goal, we formulate techniques to assimilate the latest results from helioseismology to constrain the velocity fields. We also apply mixing length theory to the Solar Model S, in conjunction with magnetic quenching of the turbulent diffusivity, to generate more realistic effective turbulent diffusivity profiles for kinematic dynamo models. In essence therefore, we try to address some of these outstanding issues in a first-principle physics based approach, rather than an ad-hoc manner.
Martens Petrus C. H.
Muñoz-Jaramillo Andrés
Nandy Dibyendu
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