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Spectroscopic Observations of Differential Rotation With Height in the Solar Envelope*

Published online by Cambridge University Press:  12 April 2016

W.C. Livingston
W.C. Livingston*
Affiliation:
Kitt Peak National Observatory†, Tucson, Ariz., U.S.A.

Abstract

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The problem of determining the spectroscopic rotation of the sun is not one of instrumental sensitivity, which can be about 10 m/sec, but rather of abstracting the rotational component from the hierarchy of long-lived surface currents. Required are continued daily observations over long periods of time and this task is not presently feasible at most observatories. Past observations have indicated a height gradient of rotational angular velocities. We have determined the photosphere and chromosphere angular velocity gradient from observations across the disk of C 5380 Å(h≃ -250 km), CN 3882 Â (h ≃ 0 km), Ca+K3(h≃+ 5000 km), together with other Fraunhofer lines of intermediate origin while K-line spectra of prominences are used to sense the chromosphere-corona interface.

Type
Part IV / The Rotation of the Sun
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 321 - 328
Copyright
Copyright © Reidel 1970

Footnotes

†

Operated by The Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.

*

Kitt Peak National Observatory Contribution No. 531.

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