Numerical simulations of sunspots

Gert Botha, Alistair Rucklidge, Neal Hurlburt

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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.
Original languageEnglish
Title of host publicationProceedings of the International Astronomical Union
EditorsF. Kupka, I. W. Roxburgh, K. L. Chan
Place of PublicationCambridge, UK
PublisherCambridge University Press
Pages507-509
Number of pages3
Volume2
ISBN (Print)9780521863490
DOIs
Publication statusPublished - 2006

Publication series

NameProceedings of the International Astronomical Union Symposia and Colloquia
PublisherCambridge University Press
ISSN (Electronic)1743-9213

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