Numerical study of compressible solar magnetoconvection with an open transitional boundary

Statistics – Computation

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Compressible Fluids, Convective Flow, Gravitational Effects, Magnetohydrodynamic Stability, Solar Corona, Solar Magnetic Field, Computerized Simulation, Hydrodynamic Equations, Magnetic Field Configurations, Magnetic Flux, Radiative Transfer

Scientific paper

Computer simulation is used to study nonlinear evolution of magnetoconvection in a system with a dynamical open boundary between the convection region and corona of the sun. A model is studied in which the fluid is subject to the vertical gravitation, MHD, and high stratification, through an MHD code with the MacCormack-Donner cell hybrid scheme in order to well represent convective phenomena. Initially the vertical fluid flux penetrates from the convectively unstable zone at the bottom into the upper diffuse atmosphere. As the instability develops, the magnetic fields are twisted by the convection motion and the folding of magnetic fields is observed. When the magnetic pressure is comparable to the thermal pressure in the upper layer of convective zone, strong flux expulsion from the convective cell interior toward the cell boundary appears. The magnetic field patterns observed are those of concentrated magnetic flux tubes, accumulation of dynamo flux near the bottom boundary, pinched flux near the downdraft region, and the surface movement of magnetic flux toward the downdraft region. Many of these computationally observed features are reminiscent of solar observations of the fluid and magnetic structures and their motions.

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