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Title:
``Energy levels and spectral lines of Ne viii'' [Eur. Phys. J. D 39, 173 188 (2006)]
Authors:
Wilhelm, K.; Curdt, W.; Dammasch, I. E.; Hassler, D. M.
Affiliation:
AA(Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany ), AB(Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany), AC(SIDC, Royal Observatory of Belgium, Circular Avenue 3, 1180 Uccle, Brussels, Belgium), AD(Southwest Research Institute, 1050 Walnut St., Suite 400, Boulder, CO 80302, USA)
Publication:
The European Physical Journal D, Volume 47, Issue 3, 2008, pp.325-325 (EPJD Homepage)
Publication Date:
05/2008
Origin:
EDP Sciences
PACS Keywords:
Fine and hyperfine structure, Ionization potentials, electron affinities, Visible and ultraviolet spectra, Atomic and molecular data, spectra, and spectral parameters
DOI:
10.1140/epjd/e2008-00057-7
Bibliographic Code:
2008EPJD...47..325W

Abstract

Kramida and Buchet-Poulizac [Eur. Phys. J. D 39, 173 (2006)] provide a comprehensive compilation of Ne VIII energy levels and spectral lines. We are concerned about the data of one line treated in the second paragraph of Section 2, the line at 77.0 nm. This line is very important for solar physics investigations as it is a bright line emitted in the lower corona of the Sun, where mass flux and energy transport determine the properties of the nascent solar wind. Consequently, it has been studied in a number of investigations, of which we want to mention two. The results are published by Peter and Judge [Astrophys. J. 522, 1148 (1999)] and Dammasch et al. [Astron. Astrophys. 346, 285 (1999)]. Both these studies concluded that the rest wavelength of the Ne VIII line in question is 77.0428 nm with standard uncertainties of 0.7 pm and 0.3 pm, respectively. Dammasch et al. discussed, in particular, the uncertainty level of 0.5 pm stated by Bockasten et al. [Proc. Phys. Soc. 81, 522 (1963)]. The conclusion was that it is far too optimistic and not reliable. So, we take issue with the statement of the authors that the Bockasten et al. measurements of this line are the most accurate in the literature. If the Bockasten et al. value (77.0409 nm ± 0.0005 nm) [Proc. Phys. Soc. 81, 522 (1963)] for the rest wavelength of this line were true, it would imply downward movements in the solar corona that are in conflict with the measurements in other lines.
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