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

  • Helioseismology
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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 article, 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.

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Authors and Affiliations

  1. Center for Turbulence Research, Stanford University, Stanford, CA, 94305, USA

    I. N. Kitiashvili

  2. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA, 94305, USA

    I. N. Kitiashvili & A. G. Kosovichev

  3. NASA Ames Research Center, Moffett Field, CA, 94035, USA

    N. N. Mansour & A. A. Wray

Authors
  1. I. N. Kitiashvili
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  2. A. G. Kosovichev
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  3. N. N. Mansour
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  4. A. A. Wray
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Corresponding author

Correspondence to I. N. Kitiashvili.

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Helioseismology

Guest Editors: G. Houdek, H. Shibahashi, and J. Zhao

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Kitiashvili, I.N., Kosovichev, A.G., Mansour, N.N. et al. Numerical MHD Simulations of Solar Magnetoconvection and Oscillations in Inclined Magnetic Field Regions. Sol Phys 268, 283–291 (2011). https://doi.org/10.1007/s11207-010-9679-0

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  • DOI: https://doi.org/10.1007/s11207-010-9679-0

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