Numerical MHD Simulations of Solar Magnetoconvection and Oscillations in Inclined Magnetic Field Regions

Abstract

The sunspot penumbra is a transition zone between the strong vertical magnetic field area (sunspot umbra) and the quiet Sun. The penumbra has a fine filamentary structure that is characterized by magnetic field lines inclined toward the surface. Numerical simulations of solar convection in inclined magnetic field regions have provided an explanation of the filamentary structure and the Evershed outflow in the penumbra. In this paper, we use radiative MHD simulations to investigate the influence of the magnetic field inclination on the power spectrum of vertical velocity oscillations. The results reveal a strong shift of the resonance mode peaks to higher frequencies in the case of a highly inclined magnetic field. The frequency shift for the inclined field is significantly greater than that in vertical field regions of similar strength. This is consistent with the behavior of fast MHD waves.

9 pages, 6 figures, Solar Physics (in press)

References in corpus (5)

• Magneto-convection in a sunspot umbra
• Solar surface emerging flux regions: a comparative study of radiative MHD modeling and Hinode SOT observations
• Local helioseismology and correlation tracking analysis of surface structures in realistic simulations of solar convection
• Traveling Waves of Magnetoconvection and the Origin of the Evershed Effect in Sunspots
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