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Solar Magneto- Convection: Structure & Dynamics Robert Stein - Mich. State Univ. Aake Nordlund - NBIfAFG

Solar Magneto-Convection: Structure & Dynamics Robert Stein - Mich. State Univ. Aake Nordlund - NBIfAFG

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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

MAGNETO-CONVECTION SIMULATIONS

QuickTime™ and aPlanar RGB decompressor

are needed to see this picture.

3D granulation

(movie by Mats Carlsson)

QuickTime™ and aYUV420 codec decompressor

are needed to see this picture.

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

Magnetic Field Lines - fed horizontally

Magnetic Field Lines - initially vertical

Flux Emergence & Disappearance1 2

3 4

Emerging flux

Disappearing flux

G-band: Center to Limb(see poster II:9)

G-band Bright Points = large B, but some large B dark

G-band image & magnetic

field contours

(-.3,1,2 kG)

Magnetic Field & Velocity (@ surface)

Magnetic Field &Velocity

High velocity sheets at

edges of flux concentration

Temperature + B contours

(1, 2, 3, kG)

Temperature &

Velocity

The End