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Realistic MHD numerical simulations of solar convection and oscillations in inclined magnetic field regions

Published online by Cambridge University Press:  21 October 2010

Irina N. Kitiashvili ,
Alexander G. Kosovichev ,
Alan A. Wray  and
Nagi N. Mansour
Irina N. Kitiashvili
Affiliation:
Center for Turbulence Research, Stanford University, Stanford, CA 94305, USA email: [email protected]
Alexander G. Kosovichev
Affiliation:
Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA email: [email protected]
Alan A. Wray
Affiliation:
Ames Research Center, Moffett Field, CA 94040, USA email: [email protected] and [email protected]
Nagi N. Mansour
Affiliation:
Ames Research Center, Moffett Field, CA 94040, USA email: [email protected] and [email protected]
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It is known that physical properties of solar turbulent convection and oscillations strongly depend on magnetic field. In particular, recent observations from SOHO/MDI revealed significant changes of the wave properties in inclined magnetic field regions of sunspots, which affect helioseismic inferences. We use realistic 3D radiative MHD numerical simulations to investigate solar convection and oscillations and their relationship in the presence of inclined magnetic field. In the case of highly inclined and strong 1-1.5 kG field the solar convection develops filamentary structure and high-speed flows (Fig. 1a), which provide an explanation to the Evershed effect in sunspot penumbra (Kitiashvili, et al. 2009).

Keywords

Sun: magnetic fieldsoscillationssunspotsconvectionturbulencemethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 348
Copyright
Copyright © International Astronomical Union 2010

References

Kitiashvili, I.N., Kosovichev, A.G., Wray, A.A. & Mansour, N.N. 2009, ApJ 700, L178CrossRefGoogle Scholar