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The Magnetic and Velocity Fields and Brightness in the Solar Atmosphere

Published online by Cambridge University Press:  14 August 2015

S. I. Gopasyuk  and
T. T. Tsap
S. I. Gopasyuk
Affiliation:
Crimean Astrophysical Observatory, Nauchny, Crimea, U.S.S.R.
T. T. Tsap
Affiliation:
Crimean Astrophysical Observatory, Nauchny, Crimea, U.S.S.R.

Abstract

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Simultaneous observations of the magnetic fields, the line-of-sight velocities and brightness were made in active and quiet regions with the Crimean double-magnetograph in the following lines: Hα, K3 Ca II, Hβ, Hγ, Hδ, MgI λ 5184 Å, CaI λ 4227 Å, D1 NaI, BaII λ 4554 Å, CaI λ 6103 Å, FeI λ 5250 Å.

It is shown, that in the active regions the horizontal velocity is larger than the vertical one.

The mean velocities in the quiet solar photosphere have an isotropic distribution (Gopasyuk and Kalman, 1971).

The mean vertical velocities increase exponentially with height in active and quiet regions.

The correlation between velocities at different levels in active and quiet regions decreases with the distance between the levels of the formation of spectral lines, and it disappears for the velocities recorded in λ 6103 Å and Hβ, for λ 5184 and Hα lines in active regions and for the velocities recorded in λ 5250 Å and Hα lines in quiet regions.

The position of the maximal field strength within a magnetic hill coincides statistically with the zero line of the line-of-sight velocities for active as well as for quiet regions.

Type
Part III: Observations of Sunspot and Active Region Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 43: Solar Magnetic Fields , 1971 , pp. 274 - 278
Copyright
Copyright © Reidel 1971 

References

Severny, A. B.: 1966, Astron. Zh. 43, 465.Google Scholar
Gopasyuk, S. I. and Kalman, B.: 1971, Izv. Krymsk. Astrofiz. Obs. 44, in press.Google Scholar