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A Quantitative Study of Magnetic Flux Transport on the Sun

Published online by Cambridge University Press:  04 August 2017

N.R. Sheeley Jr. ,
J.P. Boris ,
T.R. Young Jr. ,
C.R. DeVore  and
K.L. Harvey
N.R. Sheeley Jr.
Affiliation:
E.O. Hulburt Center for Space Research Naval Research Laboratory Washington, DC 20375
J.P. Boris
Affiliation:
Laboratory for Computational Physics Naval Research Laboratory Washington, DC 20375
T.R. Young Jr.
Affiliation:
Laboratory for Computational Physics Naval Research Laboratory Washington, DC 20375
C.R. DeVore
Affiliation:
Berkeley Research Associates Springfield, VA 22150
K.L. Harvey
Affiliation:
Solar Physics Research Corporation Tucson, AZ 85716

Abstract

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A computational model, based on diffusion, differential rotation, and meridional circulation, has been developed to simulate the transport of magnetic flux on the Sun. Using Kitt Peak magnetograms as input, we have determined a best-fit diffusion constant by comparing the computed and observed fields at later times. Our value of 730 ± 250 km2/s is consistent with Leighton's (1964) estimate of 770–1540 km2/s and is significantly larger than Mosher's (1977) estimate of 200–400 km2/s. This suggests that diffusion may be fast enough to account for the observed polar magnetic field reversal without requiring a significant assist from meridional currents.

Type
III. Theory of Stellar Magnetic Field Generation
Information
Symposium - International Astronomical Union , Volume 102: Solar and Stellar Magnetic Fields: Origins and Coronal Effects , 1983 , pp. 273 - 278
Copyright
Copyright © Reidel 1983 

References

Duvall, T.L. Jr.: 1979, Solar Phys. 63, 3.Google Scholar
Leighton, R.B.: 1964, Astrophys. J. 140, 1547.CrossRefGoogle Scholar
Mosher, J.M.: 1977, The Magnetic History of Solar Active Regions , Ph.D. Thesis, Calif. Inst. of Tech. Google Scholar