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Abstract

The work of Drobyshevski and Yuferev (1974) and Arter (1983b) is continued and extended. Magnetic flux distributions are calculated for Rayleigh-Benard convection with square planform. The importance of the local structure of the flow field near stagnation points is emphasised. When the Lorentz force is included motion often takes the form of rolls, but if three-dimensional flow persists the field distribution is essentially kinematic. Implications for dynamo and sun spot theories are discussed. These calculations do not support the use of the flux tube as conceived by Parker (1979) to model horizontal magnetic field, although this may be due to their idealized nature.

Additional information

Authors: ARTER W UNIVERSITY OF CAMBRIDGE (UK), UNIVERSITY OF CAMBRIDGE (UK); CULHAM LABORATORY, ABINGDON (UK); CULHAM LABORATORY, ABINGDON (UK), UNIVERSITY OF CAMBRIDGE (UK); CULHAM LABORATORY, ABINGDON (UK)
Bibliographic Reference: GEOPHYS. ASTROPHYS. FLUID DYNAMICS, VOL. 31 (1985), PP. 311-344
Record Number: 1989124054000 / Last updated on: 1987-01-01
Category: PUBLICATION
Available languages: en
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