Three decades of 3D global simulations of the solar dynamo (Invited)

Details Three decades of 3D global simulations of the solar dynamo (Invited) Three decades of 3D global simulations of the solar dynamo (Invited)

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh11b..01g&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH11B-01

Astronomy and Astrophysics

Astrophysics

[7544] Solar Physics, Astrophysics, And Astronomy / Stellar Interiors And Dynamo Theory

Scientific paper

Studies of convective dynamos using dynamically consistent three-dimensional numerical simulations began with the work of Gilman and Miller (1981). Their Boussinesq simulations maintained a differential rotation "constant on cylinders" and produced magnetic cycles, but with fields propagating toward the poles, unlike the sunspot cycle. Anelastic dynamo simulations then illustrated the effects of the large radial gradients in density, temperature and diffusivity (Glatzmaier 1984) and could generate fields in the overshoot region at the base of the convection zone that propagate toward the equator. However, the differential rotation was still mainly "constant on cylinders" throughout most of the convection zone. Helioseismology then showed that the sun's internal rotation profile is closer to "constant on radii", especially at mid-latitude. As computers became more powerful and parallel, more turbulent (i.e., realistic) simulations were produced (Toomre et al.), which demonstrated the importance of resolving more of the turbulent flux of angular momentum in maintaining differential rotation and generating magnetic field. Considerable progress has been made over the past three decades; but we are still far from having a clear understanding of the magnetohydrodynamics of the solar convection zone, tachocline and internal radiative region.

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