TY - GEN
T1 - Solar differential rotation
T2 - Hints to reproduce a near-surface shear layer in global simulations
AU - Guerrero, G.
AU - Smolarkiewicz, P. K.
AU - Kosovichev, A.
AU - Mansour, N.
PY - 2012/8
Y1 - 2012/8
N2 - 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.
AB - 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.
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U2 - 10.1017/S1743921313002858
DO - 10.1017/S1743921313002858
M3 - Conference contribution
AN - SCOPUS:84880531313
SN - 9781107033832
T3 - Proceedings of the International Astronomical Union
SP - 417
EP - 425
BT - Solar and Astrophysical Dynamos and Magnetic Activity
A2 - Kosovichev, Alexander G.
A2 - de Gouveia Dal Pino, Elisabete
A2 - Yan, Yihua
ER -