Computer Science
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..277g&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
1
Sun, Tachocline
Scientific paper
It is now believed that purely hydrodynamical models of the solar interior cannot explain the observed rotational structure of the radiative zone and the tachocline: a large-scale magnetic field must be present deep in the solar interior to enforce uniform rotation (Gough & McIntyre, 1998). The dynamical interaction of a rotating fluid flow with a large-scale magnetic field is a complex nonlinear phenomenon, which can be studied extensively only through numerical analysis. In this paper, I present the first numerical solutions of a dynamical axisymmetric, incompressible, steady-state MHD model of the radiative zone and the tachocline. It is found that there exists a range of values of the interior field strength for which it is possible to recover qualitatively the rotational structure of the radiative zone described by Gough & McIntyre. However, predictions for the interior angular velocity cannot reproduce the observed value; this is likely to be the result of the large magnetic diffusivity used in the simulations.
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