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Numerical simulations of stellar convective dynamos III. At the base of the convection zone

 

作者: GaryA. Glatzmaier,  

 

期刊: Geophysical & Astrophysical Fluid Dynamics  (Taylor Available online 1985)
卷期: Volume 31, issue 1-2  

页码: 137-150

 

ISSN:0309-1929

 

年代: 1985

 

DOI:10.1080/03091928508219267

 

出版商: Taylor & Francis Group

 

数据来源: Taylor

 

摘要:

We describe numerical simulations of giant-cell solar convection and magnetic field generation. Nonlinear, three-dimensional, time-dependent solutions of the anelastic magnetohydrodynamic equations are presented for a stratified, rotating, spherical shell of ionized gas. The velocity, magnetic field, and thermodynamic variables are solved simultaneously and self-consistently with full nonlinear feedback. Convection, driven in the outer part of this shell by a superadiabatic gradient, penetrates into the inner, subadiabatic part. Previous dynamic dynamo sjmulations have demonstrated that, when the dynamo operates in the convection zone, the magnetic fields propagate away from the equator in the opposite direction inferred from the solar butterfly diagram. Our simulations suggest that the solar dynamo may be operating at the base of the convection zone in the transition region between the stable interior and the turbulent convective region. There our simulated angular velocity decreases with depth, as it does in the convection zone; but the simulated helicity has the opposite sign compared to its convection zone value. As a result, our simulated magnetic fields in this transition region initially propagated toward the equator. However, due to our limited numerical resolution of the small amplitude helical fluid motions in this dense, stable region, only the initial phase propagation could be simulated, not a complete magnetic cycle.

 

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