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Axisymmetric Convection with a magnetic Field

Published online by Cambridge University Press:  15 February 2018

D. J. Galloway
D. J. Galloway*
Affiliation:
Astronomy Centre, University of Sussex, Brighton, BN1 9QH, England

Summary

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The non-linear Boussinesq equations describing axisymmetric convection in a cylinder with an initially uniform magnetic field have been integrated forward in time numerically. When the field is weak a strong central fluxrope is formed at the axis. In this case the maximum field strength can be limited either kinematically or by dynamical effects, and the equipartition prediction Bmax2 ∿ 4πμρu2 is easily exceeded. If the field is strong oscillations can occur and hysteresis is possible as the field is increased and decreased.

Type
V. Rotation and Magnetic Fields
Information
International Astronomical Union Colloquium , Volume 38: Problems of Stellar Convection , 1977 , pp. 188 - 194
Copyright
Copyright © 1976

References

Clark, A. and Johnson, A.C., 1967. Sol.Phys. 238, 433 Google Scholar
Galloway, D.J., Proctor, M.R.E., and Weiss, N.O. 1976. Nature, to be publishedGoogle Scholar
Galloway, D.J., 1976. Ph.D. Thesis, University of CambridgeGoogle Scholar
Huppert, H.E., 1976. Nature, 26338, 20 Google Scholar
Jones, C.A., Moore, D.R., and Weiss, N.O., 1976. J.Fluid Mech. 7338, 353 Google Scholar
Moore, D.R., Peckover, R.S., and Weiss, N.O., 1973. Computer Phys.Comm. 638, 198 Google Scholar
Weiss, N.O., 1966. Proc.Roy.Soc. A, 29338, 310 Google Scholar