Computer Science
Scientific paper
Oct 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.182..121b&link_type=abstract
In ESA Ultraviolet Stellar Classification p 121-130 (SEE N82-26119 16-89)
Computer Science
Classifications, Stellar Spectra, Ultraviolet Spectra, Absorption Spectra, Chemical Composition, Electron Density (Concentration), F Stars, Magnesium, Optical Resonance, Stellar Temperature
Scientific paper
Criteria for determining effective temperature and electron density independently of abundances, for A, late B, and F stars are given. Comparison of IUE data with standard classification techniques, shows that for late B and A stars, temperature classification by UV spectra is more sensitive than classification using visual spectra. The long wavelength wing of the Lyman is recommended for these stars. For A and F stars, the ratio of the Mg (2580 A) and Mg+ (2800A) resonance lines gives a good temperature/electron density (ne) criterion which is nearly independent of metal abundance (Z). The SiI discontinuities give an excellent temperature classification for A and F stars, but it is dependent on Z and ne. If the absolute intensities of either of the Mg lines are added to the criteria, three classification criteria for a three dimensional classification, according to temperature, ne and Z, are obtained.
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