Statistics – Computation
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmgp22b..08m&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #GP22B-08
Statistics
Computation
1510 Dynamo Theories, 7544 Stellar Interiors And Dynamo Theory
Scientific paper
In recent years, helioseismology has provided an unprecedented look at the dynamics of the solar interior. These new insights have been accompanied by tremendous advances in high-performance computing technology, prompting increasingly sophisticated and realistic numerical models of solar convection. Among the most important heliosesmological constraints on global-scale numerical models is the mean differential rotation profile in the solar convection zone which is established by the convection itself under the influence of rotation. I will discuss recent modeling efforts aimed at accounting for this differential rotation. Relative to earlier work which was limited by available computational resources, these more recent models are achieving more turbulent flow regimes which more closely represent the highly turbulent conditions thought to exist in the solar convection zone. Related studies have also begun to investigate the nature of supergranulation: convective patterns observed in the Solar photosphere which have a characteristic size of several angular degrees. The emphasis throughout will be on the properties of turbulent convection in rotating spherical shells. Comparable models which incorporate magnetic fields are currently in only preliminary stages but I will discuss their potential and what insight they may provide into the operation of the solar dynamo and by extension, the solar activity cycle.
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