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The Time Dependence of Magnetic, Velocity, and Intensity Fields in the Solar Atmosphere

Published online by Cambridge University Press:  14 August 2015

Neil R. Sheeley Jr.
Neil R. Sheeley Jr.*
Affiliation:
Kitt Peak National Observatory*, Tucson, Ariz. U.S.A.

Abstract

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Spectroheliogram movies of magnetic, velocity, and intensity fields have been obtained in a wide variety of spectral lines. The time resolution was typically 10–30 s. Some of the lines used were: CN λ 3883; CaI λ 6103; FeI λ 4071; FeI λ 5434; FeII λ 4924; CaII λ 3934; CaII λ 8542.

Type
Part III: Observations of Sunspot and Active Region Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 43: Solar Magnetic Fields , 1971 , pp. 310 - 315
Copyright
Copyright © Reidel 1971 

References

Chapman, G. A. and Sheeley, N. R. Jr.: 1968, Solar Phys. 5, 446.Google Scholar
Sheeley, N. R. Jr.: 1969, Solar Phys. 9, 347.Google Scholar
Sheeley, N. R. Jr. and Engvold, O.: 1969, ‘Spectroheliograms in FeII λ 4924’ , paper presented at AAS Solar Meeting, Pasadena, Calif., Febr. 18–21, 1969.Google Scholar
Sheeley, N. R. Jr. and Engvold, O.: 1970, Solar Phys. 12, 75.Google Scholar
Vrabec, D.: 1971, this volume, p. 329.CrossRefGoogle Scholar