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

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Presentation transcript:

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: T min Mm below surface, 6x6 Mm horizontally

METHOD

Conservation Equations Mass Momentum Energy Magnetic Flux

Radiation Transfer LTE Non-gray Formal Solution Calculate J - B by integrating Feautrier equations along one vertical and 4 slanted rays through each grid point on the surface. Produces low entropy plasma whose buoyancy work drives convection

5 Rays Through Each Surface Grid Point Interpolate source function to rays at each height

Opacity is binned, according to its magnitude, into 4 bins.

Solve Transfer Equation for each bin i

MAGNETO- CONVECTION SIMULATIONS

3D granulation (movie by Mats Carlsson)

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 & Disappearance 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

Magnetic Field & Velocity

Temperature & Magnetic Field (contours 1, 2 kG)

Temperature & Velocity

Temperature Gradients largest next to magnetic concentrations

Magnetic concentrations: cool, low  low opacity. Towards limb, radiation emerges from hot granule walls behind. On optical depth scale, magnetic concentrations are hot, contrast increases with opacity

Micropore Formation Small granule is squeezed out of existence Magnetic flux moves into location of previous granule

The End