A solar spectral line list between 10 and 200 A modified for application to high spectral resolution X-ray astronomy

Details A solar spectral line list between 10 and 200 A modified for application to high spectral resolution X-ray astronomy A solar spectral line list between 10 and 200 A modified for application to high spectral resolution X-ray astronomy

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apjs...56...67d&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 56, Sept. 1984, p. 67-89. Navy-NASA-supported research.

Astronomy and Astrophysics

Astronomy

49

Line Spectra, Solar Spectra, Solar X-Rays, Space Plasmas, X Ray Astronomy, Binary Stars, Emission Spectra, High Resolution, Plasma Spectra, Spectral Resolution, Stellar Spectra, X Ray Sources, X Ray Spectroscopy

Scientific paper

A spectral line list for the 10-200 A range is developed from existing solar spectra for application to high spectral resolution measurements of astrophysical plasmas. The solar spectral line lists are merged into a single comprehensive list. The effect of the solar emission measure distribution is removed from the line intensities, which results in a set of emission rates for the lines that can be applied to many optically thin, low density high temperature plasmas in ionization equilibrium. In addition to the measured solar lines, 250 theoretical lines are added to this list. These lines fall in wavelength regions where the existing solar lists have few lines because of limitations in instrumental sensitivity. Also, some lines have been added because the sun has very little plasma at temperatures of about one million K, and consequently these lines are weak or absent in solar spectra. The entire list contains about 600 lines. Finally, predicted spectra of the two RS CVn stars, alpha Aur (Capella) and UX Ari, are presented at 1 and 0.25 A spectral resolution. Also, the solar spectrum is shown at 1 A resolution, and the emission rate spectrum (spectrum not modified by an emission measure distribution) is shown at very high spectral resolution. The predicted spectra for Capella and UX Ari are based on results obtained from the Einstein and International Ultraviolet Explorer (IUE) spacecraft.

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