Statistics – Computation
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp33a..01n&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SP33A-01
Statistics
Computation
2162 Solar Cycle Variations (7536), 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162), 7537 Solar And Stellar Variability (1650), 7544 Stellar Interiors And Dynamo Theory
Scientific paper
In the kinematic approach to solar dynamo modeling, one solves for the mean magnetic field with given velocity fields such as differential rotation and meridional circulation; in addition, key physical processes such as turbulent diffusion, magnetic buoyancy and the dynamo α-effect have to be parameterized appropriately. Kinematic dynamo models perhaps do not capture the full range of complexities of stellar convection zones and approximates complex processes through simple parameterizations. Nevertheless, the underlying physics of this class of models is relatively more transparent, they are computationally less demanding and they successfully explain many observed features of the solar cycle. In this lecture, I will trace the historical development of solar kinematic dynamo models, describe the basic physical ingredients and observational inputs necessary to build one, present our current state of understanding, and highlight outstanding problems.
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