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Preliminary Results of Spectroscopic Determination of the Coronal Rotation

Published online by Cambridge University Press:  14 August 2015

V. E. Stepanov  and
N. F. Tjagun
V. E. Stepanov
Affiliation:
Siberian Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Irkutsk, U.S.S.R.
N. F. Tjagun
Affiliation:
Siberian Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Irkutsk, U.S.S.R.

Abstract

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Coronal rotation is determined by means of the spectroscopic method. The mean value of the rotation rate vs. the heliographic latitude is found. At high latitudes the corona rotates much faster than the underlying photosphere. This fact confirms Waldmeier's and Billing's hypothesis that the high-latitude phenomena should depend on the magnetic fields of low latitudes and that the interchange of the matter between the active zone and polar coronal region along the field lines should take place.

Type
Part VI: Optical and Radio Observations of Large Scale Magnetic Fields on the Sun
Information
Symposium - International Astronomical Union , Volume 43: Solar Magnetic Fields , 1971 , pp. 667 - 671
Copyright
Copyright © Reidel 1971 

References

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