Magnetohydrodynamic 3-D Models of the Solar Convection Zone

Details Magnetohydrodynamic 3-D Models of the Solar Convection Zone Magnetohydrodynamic 3-D Models of the Solar Convection Zone

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13...94b&link_type=abstract

Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 July

Astronomy and Astrophysics

Astronomy

Scientific paper

We discuss recent progresses made in modelling the complex magnetohydrodynamics of the Sun using our anelastic spherical harmonics (ASH) code on massively parallel computers. We have conducted 3--D MHD simulations of compressible convection in spherical shells to study the coupling between convection rotation and magnetic field in seeking to understand how the solar differential rotation is established and maintained. The resulting convection within domains that capture a good fraction of the bulk of the solar convection zone is highly time dependent and intricate and is dominated by intermittent upflows and networks of strong downflows (i.e. plumes). These plumes play a significant role in yielding Reynolds stresses that serve to redistribute angular momentum leading to angular velocity profiles that make good contact with helioseismic deductions. Such complex convective flows are efficient in amplifying the magnetic energy near equipartition. The resulting magnetic fields are found to concentrate around the downflowing networks and to have significant north-south asymmetry and helicity. But these strong fields yield Maxwell stresses that seek to speed up the poles and destroy the agreement with helioseismic observations. So for a given angular velocity profile the level of magnetism that the Sun can sustain is likely to be limited.

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