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Influence of magnetic fields on the structure of the solar corona∗

Published online by Cambridge University Press:  14 August 2015

G. Newkirk ,
M. D. Altschuler  and
J. Harvey
G. Newkirk
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colo., U.S.A.
M. D. Altschuler
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colo., U.S.A.
J. Harvey
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colo., U.S.A.

Abstract

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A current-free approximation to the coronal magnetic field is calculated from measured photospheric magnetic fields (Mt. Wilson) and traced by computer. The calculated field structure is then compared to a white-light photograph of the November 12, 1966 eclipse.

Type
Part V: Coronal and Interplanetary Structure of an Active Region
Information
Symposium - International Astronomical Union , Volume 35: Structure and Development of Solar Active Regions , 1968 , pp. 379 - 384
Copyright
Copyright © Reidel 1968 

References

Chapman, S., Bartels, J. (1940) Geomagnetism, Oxford University Press, London.Google Scholar
Malitson, H. H., Erickson, W.C. (1966) Astrophys. J., 144, 337.Google Scholar
Meyer, F., Schmidt, H. (1966) Mitt. Astron. Geos., 21.Google Scholar
Newkirk, G. (1967) Annual Rev. Ast. and Ap., 5, 213.Google Scholar
Whang, Y.C., Liu, C.K., Chang, C.C. (1966) Astrophys. J., 145, 255.Google Scholar