Solar Magneto-Convection:Structure & Dynamics
Robert Stein - Mich. State Univ.
Aake Nordlund - NBIfAFG
METHOD• Solve conservation equations for:
mass, momentum, internal energy & induction equation for vector potential
• Radiative heating/cooling -- solve Feautrier transfer equation, LTE, 4 opacity bins, 1 vertical & 4 slanted rays
• EOS includes ionization, excitation
• Simulation domain: Tmin - 2.5 Mm below
surface, 6x6 Mm horizontally
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3D granulation
(movie by Mats Carlsson)
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B Swept to Cell Boundaries
Boundary Conditions
Magnetic structure depends on boundary conditions
1) Inflows at bottom advect horizontal field in
2) At bottom: boundary magnetic field vertical • At top: B tends toward potential
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