In Convection in Astrophysics (IAU S239) (eds. F. Kupka, I.W. Roxburgh and K.L. Chan) Cambridge University Press (2006).

Numerical simulations of sunspots

G.J.J. Botha(1), A.M.Rucklidge(1) and N.E. Hurlburt(2)
(1) Department of Applied Mathematics,
University of Leeds, Leeds LS2 9JT, UK

(2) Lockheed Martin Solar and Astrophysics Laboratory,
Organization L9-41 Building 252, Palo Alto, CA 94304, USA

Abstract. The origin, structure and evolution of sunspots are investigated using a numerical model. The compressible MHD equations are solved with physical parameter values that approximate the top layer of the solar convection zone. A three dimensional (3D) numerical code is used to solve the set of equations in cylindrical geometry, with the numerical domain in the form of a wedge. The linear evolution of the 3D solution is studied by perturbing an axisymmetric solution in the azimuthal direction. Steady and oscillating linear modes are obtained.

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