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Solar rotation in the chromosphere and corona

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Abstract

Extreme ultraviolet spectroheliograms in Mg x (625 Å) and the Lyman continuum (897 Å) obtained from OSO-6 are used to determine the differential rotation rate in the solar chromosphere and corona. The equatorial rotation rate agrees with spectroscopic measurements of the photospheric plasma velocity; the variation of rate with latitude is less pronounced than in most other determinations. We cannot discern a variation in the rotation rate between the chromosphere and corona.

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Author notes

  1. William Henze Jr.

    Present address: Teledyne Brown Engineering, 35807, Research Park, Huntsville, Ala., U.S.A

Authors and Affiliations

  1. Center for Astrophysics, Harvard College Observatory and Smithsonian Astrophysical Observatory, 02138, Cambridge, Mass., U.S.A

    William Henze Jr. & A. K. Dupree

Authors
  1. William Henze Jr.
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  2. A. K. Dupree
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Henze, W., Dupree, A.K. Solar rotation in the chromosphere and corona. Sol Phys 33, 425–429 (1973). https://doi.org/10.1007/BF00152429

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  • DOI: https://doi.org/10.1007/BF00152429

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