Numerical simulations of sunspots
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.
- Publication:
-
Convection in Astrophysics
- Pub Date:
- May 2007
- DOI:
- Bibcode:
- 2007IAUS..239..507B
- Keywords:
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- (magnetohydrodynamics:) MHD;
- Sun: magnetic fields;
- sunspots