𝔖 Bobbio Scriptorium
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Coronal emission line profile observations at total solar eclipses

✍ Scribed by D. H. Liebenberg; R. J. Bessey; B. Watson

Publisher
Springer
Year
1975
Tongue
English
Weight
834 KB
Volume
44
Category
Article
ISSN
0038-0938

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✦ Synopsis

High resolution spectra of the coronal emission line Fe xIv at 530.3 nm obtained at the 30 May 1965 total solar eclipse are analyzed and interpreted. Deconvolution techniques that preserve the line intensity vs wavelength profile shape are developed to obtain further resolution improvement. The west limb coronal enhancement is determined to have temperatures less than 3 MK and turbulent velocities of N25 km s -1 decreasing with altitude. Temperature gradients provide evidence for marginal solar wind flow from this enhancement. Above the quiet photosphere in the southwest quadrant the comparison of line and continuum intensities and consideration of line width suggest to us tbe coronal region is filled with inhomogeneous plasma, dense enough in localized regions to maintain collisional excitation. Solar wind flow from this region obtains when turbulent velocities are assumed to contribute to the line broadening. We identify this region as a coronal hole apd suggest that coronal material is heated by the quiet photosphere below.

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