Line identifications in stars of spectral type SC

Details Line identifications in stars of spectral type SC Line identifications in stars of spectral type SC

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apjs...71..341w&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 71, Oct. 1989, p. 341-355.

Other

10

Abundance, Carbon Stars, Line Spectra, S Stars, Stellar Spectra, Astronomical Photography, Heavy Elements, Nuclear Fusion, Spectrum Analysis, Tables (Data)

Scientific paper

Results of line identifications from 6.7 A/mm photographic image-tube spectra of the SC star CY Cyg are presented, and line intensities are compared with those in six other SC stars. A comparison of CY Cyg with two other SC stars, GP Ori and FU Mon, indicates that the lines most frequently enhanced in the two cooler stars arise from Ti I, La I, and Zr I. Line identifications and estimates of intensity are not sufficient to dissociate effects of temperature and abundance. However, it appears that La is exceptionally enhanced as compared with other elements and is very likely to be in higher abundance in GP Ori and FU Mon relative to CY Cyg. Lines of Ba I indicate that Ba may also be enhanced in the same two stars. The technetium line at 5924.47 A is probably present in all the stars except BD +38 deg 955 but is broadened by hyperfine structure and blended with lines of Ti, V I, and CN. Lines of europium are not strong, and may not even be present, indicating that the anomalously strong lines of heavy elements have been produced by s-processing and have been mixed to the surface within a few half-lives of Tc-99 , i.e., (0.5 - 1.0) x 10 to the 6th yr.

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