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Concentration of magnetic fields in the deep convection zone

Published online by Cambridge University Press:  14 August 2015

G. W. Simon  and
N. O. Weiss
G. W. Simon
Affiliation:
Sacramento Peak Observatory, Sunspot, N.M., U.S.A.
N. O. Weiss
Affiliation:
Dept. of Applied Mathematics and Theoretical Physics, Silver Street, Cambridge, England

Abstract

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The strong magnetic fields observed between supergranules indicate that there must be subphotospheric convection in cells with a preferred diameter of about 30000 km. Orthodox mixing length theory assumes that the dimensions of cells are limited by the density scale-height. This is adequate for explaining granules but cannot account for supergranulation. A model is therefore proposed in which cellular motions extend over several scale-heights. In addition to granules and supergranules this model predicts a third characteristic scale of motion, with giant cells around 300000 km in diameter. These cells may produce a pattern of magnetic fields like that suggested by Bumba and Howard for complexes of activity.

Type
Part II: Theoretical Aspects
Information
Symposium - International Astronomical Union , Volume 35: Structure and Development of Solar Active Regions , 1968 , pp. 108 - 111
Copyright
Copyright © Reidel 1968 

References

Bumba, V., Howard, R. F. (1965a) Astrophys. J., 141, 1492.CrossRefGoogle Scholar
Bumba, V., Howard, R. F. (1965b) Astrophys. J., 141, 1502.CrossRefGoogle Scholar
Sheeley, N.R. Jr. (1966) Astrophys. J., 144, 723.CrossRefGoogle Scholar
Simon, G.W., Weiss, N.O. (1968) to be published.Google Scholar