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Interpretation of XUV spectroheliograms

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Abstract

Some parameters of chromospheric structure are drawn from recently published XUV spectroheliograms. The HeII emission above the limb arises from the small amount of He+ still existing at 106°. The larger amounts of He+ in the cooler corona at the poles explain the polar cap absorption in λ 304. The flat distribution of emission in Oiv and Ov, with a sharp spike at the limb, is caused by the rough structure of the chromosphere and the variable excitation in the emitting spicules. The intensity of the Nevii lines shows that the transition zone between chromosphere and corona is very sharp.

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Authors and Affiliations

  1. Mount Wilson and Palomar Observatories, Carnegie Institution of Washington, California Institute of Technology, U.S.A.

    Harold Zirin

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  1. Harold Zirin
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This research was supported by the National Aeronautics and Space Administration under Grant NASA NGR 05 002 034.

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Zirin, H. Interpretation of XUV spectroheliograms. Sol Phys 9, 77–87 (1969). https://doi.org/10.1007/BF00145730

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  • DOI: https://doi.org/10.1007/BF00145730

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