The solar spectrum: wavelengths and identifications from 160 to 770 Ångstroms.
Abstract
The full-Sun solar spectrum from 160 to 770 A was photographed under quiet solar conditions by a rocket-borne spectrograph flown in 1973 September. The spectral resolution is 0.06 A or better. We present a composite list of spectral lines, including wavelengths, identifications, and approximate intensities that were obtained from the present flight and from a previous flight in 1969 May. This line list contains the most accurate solar wavelengths yet obtained in this spectral region. One result is improved energy levels which are given for the two lowest energy configurations of Fe ix through Fe xvi. No detectable relative mass motions of more than 4 km s ' exist between transition zone and coronal regions averaged over the visible disk of the Sun. The wavelengths of emission lines in this spectrum were determined with indicated accuracies ranging between 2 and 20 mA. The spectrograph employed a 3 m radius, 600 grooves mm ' gold grating used at grazing incidence. Subject headings: line identifications - Sun: corona - Sun: spectra - ultraviolet: spectra
- Publication:
-
The Astrophysical Journal
- Pub Date:
- January 1976
- DOI:
- 10.1086/154107
- Bibcode:
- 1976ApJ...203..521B
- Keywords:
-
- Rocket-Borne Instruments;
- Solar Spectra;
- Spectral Line Width;
- Spectrum Analysis;
- Ultraviolet Spectra;
- Aerobee Rocket Vehicle;
- Atomic Energy Levels;
- Electron Transitions;
- Luminous Intensity;
- Reentry Effects;
- Solar Activity;
- Solar Corona;
- Tables (Data);
- Wavelengths;
- Solar Physics