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Numerical simulations of sunspots

Published online by Cambridge University Press:  01 August 2006

G. J. J. Botha ,
A. M. Rucklidge  and
N. E. Hurlburt
G. J. J. Botha
Affiliation:
Department of Applied Mathematics, University of Leeds, Leeds LS2 9JT, UK email: gert@maths.leeds.ac.uk; A.M.Rucklidge@leeds.ac.uk
A. M. Rucklidge
Affiliation:
Department of Applied Mathematics, University of Leeds, Leeds LS2 9JT, UK email: gert@maths.leeds.ac.uk; A.M.Rucklidge@leeds.ac.uk
N. E. Hurlburt
Affiliation:
Lockheed Martin Solar and Astrophysics Laboratory, Organization L9-41, Building 252, Palo Alto, CA 94304, USA email: hurlburt@lmsal.com
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Abstract

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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.

Keywords

(magnetohydrodynamics:) MHDSun: magnetic fieldssunspots

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 507 - 509
Copyright
Copyright © International Astronomical Union 2007

References

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