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Investigation of Coronal Rotation by the Spectroscopic Method

Published online by Cambridge University Press:  14 August 2015

V. E. Stepanov  and
N. F. Tjagun
V. E. Stepanov
Affiliation:
Sibizmiran, Irkutsk, U.S.S.R.
N. F. Tjagun
Affiliation:
Sibizmiran, Irkutsk, U.S.S.R.

Abstract

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Coronal rotation is different in the northern and southern hemispheres of the Sun and varies with the cycle of solar activity. A sharp decrease in linear velocity by 0.4 km s−1 on the latitude and its relative constancy in the latitude interval 35° < φ < 50° are the most typical.

In the southern polar region an intensive stream of coronal gas directed oppositely to the solar rotation was detected during the time interval 1969–1972. In the greater part of the latitude range, on average, the corona rotates more slowly in comparison with the solar atmosphere at the photospheric level.

Type
Part 1: Basic Observed Parameters of the Solar Cycle
Information
Symposium - International Astronomical Union , Volume 71: Basic Mechanisms of Solar Activity , 1976 , pp. 101 - 106
Copyright
Copyright © Reidel 1976 

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