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Large-Scale Flow Patterns in the Solar Atmosphere

Published online by Cambridge University Press:  19 July 2016

K.R. Sivaraman
K.R. Sivaraman*
Affiliation:
Indian Institute of Astrophysics Bangalore 560034 INDIA

Extract

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It is now well established (McIntosh 1979; Makarov and Sivaraman 1983) that the filament and filament channels seen in the H-alpha spectroheliograms (or filtergrams) can be used as reliable tracers for studying the time evolution of large-scale magnetic fields on the Sun. These features represent the neutral lines between the unipolar regions of opposite polarity. Comparison of the synoptic charts compiled from H-alpha pictures with those from full-disc magnetograms for the same period shows very good agreement and hence the former can be used with confidence for time evolution studies of large-scale unipolar regions for those periods when the magnetographs did not even exist. In this paper we shall present one of the results of our study (Makarov and Sivaraman 1983, 1989) on the migration of H-alpha filaments, namely, the existence of the meridional flow on the Sun. We shall extend it further to show the participation of this meridional flow in the solar cycle variation.

Type
IV. Photospheric Flows and Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 101 - 105
Copyright
Copyright © Kluwer 1990 

References

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