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Realistic MHD simulations of magnetic self-organization in solar plasma

Published online by Cambridge University Press:  08 June 2011

I. N. Kitiashvili ,
A. G. Kosovichev ,
A. A. Wray  and
N. N. Mansour
I. N. Kitiashvili
Affiliation:
Center for Turbulence Research, Stanford University, Stanford, CA 94305, USA email: irinasun@stanford.edu W.W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
A. G. Kosovichev
Affiliation:
W.W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
A. A. Wray
Affiliation:
Center for Turbulence Research, Stanford University, Stanford, CA 94305, USA email: irinasun@stanford.edu NASA Ames Research Center, Moffett Field, Mountain View, CA 94040, USA
N. N. Mansour
Affiliation:
Center for Turbulence Research, Stanford University, Stanford, CA 94305, USA email: irinasun@stanford.edu NASA Ames Research Center, Moffett Field, Mountain View, CA 94040, USA
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Abstract

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Filamentary structure is a fundamental property of the magnetized solar plasma. Recent high-resolution observations and numerical simulations have revealed close links between the filamentary structures and plasma dynamics in large-scale solar phenomena, such as sunspots and magnetic network. A new emerging paradigm is that the mechanisms of the filamentary structuring and large-scale organization are natural consequences of turbulent magnetoconvection on the Sun. We present results of 3D radiative MHD large-eddy simulations (LES) of magnetic structures in the turbulent convective boundary layer of the Sun. The results show how the initial relatively weak and uniformly distributed magnetic field forms the filamentary structures, which under certain conditions gets organized on larger scales, creating stable long-living magnetic structures. We discuss the physics of magnetic self-organization in the turbulent solar plasma, and compare the simulation results with observations.

Keywords

PlasmasturbulenceSun: granulationmagnetic fieldssunspotsphotosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 120 - 124
Copyright
Copyright © International Astronomical Union 2011

References

Evershed, J. 1909, MNRAS, 69, 454Google Scholar
Jacoutot, L., Kosovichev, A. G., Wray, A., & Mansour, N. N. 2008, ApJ, 682, 1386.Google Scholar
Kitiashvili, I. N., Kosovichev, A. G., Wray, A. A., & Mansour, N. N. 2009, ApJ, 700, L178.Google Scholar
Kitiashvili, I. N., Bellot Rubio, L. R., Kosovichev, A. G., Mansour, N. N., Sainz Dalda, A., & Wray, A. A. 2010a, ApJ, 716, L181.Google Scholar
Kitiashvili, I. N., Kosovichev, A. G., Wray, A. A., & Mansour, N. N. 2010b, Proc. of 3rd Hinode Science Meeting, 1-4 December, 2009, in press.Google Scholar
Kitiashvili, I. N., Kosovichev, A. G., Wray, A. A., & Mansour, N. N. 2010c, ApJ, 719, 307.Google Scholar
Stein, R. F. & Nordlund, Å. 1989, ApJ, 342, L95CrossRefGoogle Scholar