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Holes in the Solar Corona

Published online by Cambridge University Press:  14 August 2015

W. M. Glencross
W. M. Glencross*
Affiliation:
Mullard Space Science Laboratory, Dept. of Physics and Astronomy, University College London, WC1E 6BT, England

Summary

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Babcock (1961) outlined the sequence of events which takes place in the Sun's atmosphere during a solar cycle. Magnetic field loops, having preferred directions, emerge from the solar surface and thereafter merge with neighbouring loops to produce more extended structures. Although flux tubes emerge with a strong E-W field component, having the field direction reversed from one side of the equator to the other, there is a tendency for the longer loops produced by merging to have a significant N-S alignment (Hansen et al., 1972).

Type
Part 1: General Solar Activity, Coronal Holes and Bright Points
Information
Symposium - International Astronomical Union , Volume 68: Solar X, Gamma, and EUV Radiation , 1975 , pp. 19 - 21
Copyright
Copyright © Reidel 1975 

References

Babcock, H. W.: 1961, Astrophys. J. 133, 572.Google Scholar
Hansen, S. F., Hansen, R. T., and Garcia, C. J.: 1972, Solar Phys. 26, 202.Google Scholar
Ioshpa, B. A.: 1968, in Kiepenheuer, K. O. (ed.), ‘Structure and Development of Solar Active Regions’, IAU Symp. 35, 261.Google Scholar
Vaiana, G. S., Kreiger, A. S., and Timothy, A. F.: 1973, Solar Phys. 32, 81.Google Scholar