Numerical simulation of near surface solar magnetoconvection

Making numerical simulations of convective flows in the solar atmosphere, we want to study the origin of the magnetic fields in the quiet solar atmosphere. The global magnetic field of the sun is produced by an interaction between convective flows in the solar interior and the rotation of the sun. The solar magnetic field is responsible for all solar activity phenomena such as sun spots. However, magnetic fields occur also in quiet regions of the solar surface. The origin of these magnetic fields is not well established. Numerical simulations make it plausible that the magnetic field in the quiet regions is produced by a local dynamo mechanism. Hence these simulations use only a simple model for the convective flows, numerical simulations with more realistic physics are required to clarify this point. The target of this project is the numerical simulation of convective flows in the solar atmosphere including magnetic fields with realistic models for the convection. The simulations are done using an existing computer program at the Astrophysical Institute Potsdam. The program treats three-dimensional, compressible convection using a realistic equation of state for the solar plasma, and direct treatment of the radiation transfer. In present state, the code does not consider magnetic fields. Therefore, the code will be extended to include magnetic fields during the duration of the project.