Solar Magneto-Convection Simulations

Robert F. Stein (1), David Benson (1) Aake Nordlund (2) Dali Georgobiani (2)

(1) Michigan State University
(2) Copenhagen University

We review the recent solar magneto-convection simulations and comment on their implications for dynamo action. Magneto-convection has been simulated in the deep convection zone on global scales, as well as near the solar surface (including realistic physics) on small (meso-granule) scales. The emergence of magnetic flux through the solar surface into the corona has begun to be modeled. In addition, realistic, non-magnetic simulations on supergranule scales (48 Mm x 20 Mm) including f-plane rotation have begun and will, once magnetic fields are included, provide information of the origin and maintenance of the magnetic network.

Correspondence

Robert F. Stein (stein@pa.msu.edu), Michigan State University

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