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Solar differential rotation: hints to reproduce a near-surface shear layer in global simulations

Published online by Cambridge University Press:  18 July 2013

G. Guerrero ,
P. K. Smolarkiewicz ,
A. Kosovichev  and
N. Mansour
G. Guerrero
Affiliation:
Solar Physics, HEPL, Stanford University, 452 Lomita mall, Stanford, CA, 94305-4085 email: guerrero@stanford.edu, sasha@sun.stanford.edu
P. K. Smolarkiewicz
Affiliation:
National Center for Atmospheric Research, Boulder, CO, 80307, USA email: smolar@ucar.edu
A. Kosovichev
Affiliation:
Solar Physics, HEPL, Stanford University, 452 Lomita mall, Stanford, CA, 94305-4085 email: guerrero@stanford.edu, sasha@sun.stanford.edu
N. Mansour
Affiliation:
NASA Ames Research Center, Moffett Field, Mountain View, CA 94040, USANagi.N.Mansour@nasa.gov
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Abstract

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Convective turbulent motions in the solar interior, as well as the mean flows resulting from them, determine the evolution of the solar magnetic field. With the aim to get a better understanding of these flows we study anelastic rotating convection in a spherical shell whose stratification resembles that of the solar interior. This study is done through numerical simulations performed with the EULAG code. Due to the numerical formulation, these simulations are known as implicit large eddy simulations (ILES), since they intrinsically capture the contribution of, non-resolved, small scales at the same time maximizing the effective Reynolds number. We reproduce some previous results and find a transition between buoyancy and rotation dominated regimes which results in anti-solar or solar like rotation patterns. Even thought the rotation profiles are dominated by Taylor-Proudman columnar rotation, we are able to reproduce the tachocline and a low latitude near-surface shear layer. We find that simulations results depend on the grid resolution as a consequence of a different sub-grid scale contribution.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 417 - 425
Copyright
Copyright © International Astronomical Union 2013 

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