Mean flows in rotating turbulent convective shells

Details Mean flows in rotating turbulent convective shells Mean flows in rotating turbulent convective shells

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..619b&link_type=abstract

In: Proceedings of the SOHO 10/GONG 2000 Workshop: Helio- and asteroseismology at the dawn of the millennium, 2-6 October 2000,

Computer Science

6

Sun: Differential Rotation, Numerical Simulations

Scientific paper

We conduct numerical simulations of turbulent compressible convection within rotating spherical shells to model solar differential rotation and meridional circulation. These 3-D simulations are carried out on massively parallel computers using the Anelastic Spherical Harmonic (ASH) code. The evolution of such convection is studied in four cases which sample several paths in achieving highly turbulent flows that are able to drive a strong differential rotation from equator to pole. The resulting angular velocity Ω profiles make reasonable contact with many aspects of the solar rotation profiles inferred from helioseismic inversions of both MDI and GONG data. The substantial contrast in Ω of order 30% achieved in our simulations of turbulent convection is considerably greater than realized in previous studies.

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