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Structure within a Magnetic Flux Tube

Published online by Cambridge University Press:  25 April 2016

P. R. Wilson
P. R. Wilson*
Affiliation:
Department of Applied Mathematics, University of Sydney
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Extract

Since their initial discovery by Hale, the nature of solar magnetic fields has presented us with a number of problems. At one time it was thought that the field consisted of a weak background dipole field of order 1-2 G on which was superimposed the considerably more intense fields associated with active regions and sunspots. However, more recent observational studies by Harvey, Frasier, Stenflo and others have suggested that 90% of the background field appears in the form of intense small-scale fields with intensities of order 103 gauss or greater and which have remarkably similar properties whether they occur in active or quiet regions. In particular, the field intensity appears independent of the total amount of flux present but the appearance of the structure depends critically on the total flux.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 3 , Issue 3 , 1978 , pp. 225 - 226
Copyright
Copyright © Astronomical Society of Australia 1978

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References

Parker, E. N., Astrophys. J., 204, 259 (1976).Google Scholar
Parker, E. N., Astrophys. J., 214, 616 (1977).CrossRefGoogle Scholar
Simon, G. W. and Weiss, N. O., Solar Phys., 13, 85 (1970).Google Scholar
Wilson, P. R., Astrophys. J., 214, 611 (1977).Google Scholar