Abstract
The utility of very high dispersion spectra (5–11 mm/Å) for the study of line profile and velocity structure in quiescent prominences is demonstrated by observations, taken with the spectregraphic slit positioned normal to the limb in Hα λ6563 Å, He D3 λ5876 Å, and Ca+K λ3933 Å. The emission profiles of both Hα and the K line often show a central reversal (absorption). Emission structures in the K-line can be complex with details as narrow as 0.04 Å. Frequently this structure consists of two distinct components: a central, strong, rather narrow line, and an often displaced, weak feature of undefined profile appearing as ‘fuzz’. It is suggested that this fuzz indicates an exchange of matter between the prominence and the corona.
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Visiting Astronomer, Institute for Theoretical Astrophysics, Oslo, Norway.
Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.
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Engvold, O., Livingston, W. High dispersion spectroscopic study of quiescent prominences. Sol Phys 20, 375–388 (1971). https://doi.org/10.1007/BF00159770
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DOI: https://doi.org/10.1007/BF00159770