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Magnetohydrodynamic Simulation of the Evolution of Bipolar Magnetic Regions

Published online by Cambridge University Press:  12 April 2016

S. T. Wu ,
C. L. Yin ,
P. Mcintosh  and
E. Hildner
S. T. Wu
Affiliation:
Center for Space Plasma and Aeronomic Research and Department of Mechanical Engineering The University of Alabama in Huntsville Huntsville, Alabama 35899U.S.A.
C. L. Yin
Affiliation:
Center for Space Plasma and Aeronomic Research and Department of Mechanical Engineering The University of Alabama in Huntsville Huntsville, Alabama 35899U.S.A.
P. Mcintosh
Affiliation:
Space Environment Laboratory, National Oceanic and Atmospheric Administration, Boulder, Colorado 80303U.S.A.
E. Hildner
Affiliation:
Space Environment Laboratory, National Oceanic and Atmospheric Administration, Boulder, Colorado 80303U.S.A.

Abstract

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It has been recognized that the magnetic flux observed on the solar surface appears first in low latitudes, and then this flux is gradually dispersed by super granular convective motions and meridional circulation. Theoretically, the magnetic flux transport could be explained by the interactions between magnetic fields and plasma flows on the solar surface through the theory of magnetohydrodynamics.

To understand this physical scenario, a quasi-three-dimensional, time-dependent, MHD model with differential rotation, meridional flow and effective diffusion as well as cyclonic turbulence effects is developed. Numerical experiments are presented for the study of Bipolar Magnetic Regions (BMRs). When the MHD effects are ignored, our model produced the classical results (Leighton, Astrophys. J., 146, 1547, 1964). The full model’s numerical results demonstrate that the interaction between magnetic fields and plasma flow (i.e., MHD effects), observed together with differential rotation and meridional flow, gives rise to the observed complexity of the evolution of BMRs.

Type
Session 2. Theory of Active Region Structure
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 98 - 107
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

1. DeVore, C. Richard, Sheeley, N. R. Jr., Boris, J. P., Young, R. T. Jr., and Harvey, K. L.: 1984, Solar Phys. 92, 1.Google Scholar
2. DeVore, C. R., Sheeley, N. R. Jr., Boris, J. P., Young, R. T. Jr., and Harvey, K. L.: 1985 Solar Phys. 102, 41.Google Scholar
3. DeVore, C. R., and Sheeley, N. R. Jr.: 1987 Solar Phys. 108, 47.Google Scholar
4. Leighton Robert, B.: 1964, Ap.J. 140, 1547.CrossRefGoogle Scholar
5. Mclntosh, P. S. and Wilson, P. R.: 1985, Solar Phys. 97, 59.Google Scholar
6. Parker, E.N., Cosmic Magnetic Fields, Oxford University Press, England, p. 509, 1979.Google Scholar
7. Sheeley, N. R. Jr., DeVore, C. R., and Boris, J. P.: 1985 Solar Phys. 98, 219.CrossRefGoogle Scholar
8. Sheeley, N. R. Jr., and DeVore, C. R.: 1986, Solar Phys. 103, 203.CrossRefGoogle Scholar
9. Wang, H.: 1988, Solar Phys. 116, 1.Google Scholar
10. Wang, Y.-M. and Sheeley, N. R. Jr.: 1991, Ap. J. 375, 761.Google Scholar
11. Wilson, P. R.: 1986, Solar Phys. 106, 1.CrossRefGoogle Scholar
12. Wilson, P. R. and Mclntosh, P. S.: 1991 Solar Phys. 136, 221.CrossRefGoogle Scholar