Spectral synthesis in the ultraviolet. III - The spectral morphology of normal stars in the mid-ultraviolet

Details Spectral synthesis in the ultraviolet. III - The spectral morphology of normal stars in the mid-ultraviolet Spectral synthesis in the ultraviolet. III - The spectral morphology of normal stars in the mid-ultraviolet

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...364..272f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 364, Nov. 20, 1990, p. 272-294.

Astronomy and Astrophysics

Astronomy

40

Astronomical Spectroscopy, Stellar Spectra, Ultraviolet Astronomy, Abundance, Cool Stars, Metallicity, Spectral Energy Distribution, Star Formation, Stellar Temperature

Scientific paper

The morphology of 218 mid-UV spectra of stars ranging from O through K in spectral type is examined. Several new line and continuum indices are defined and their usefulness as temperature, luminosity, and metallicity discriminants is discussed. Mid-UV stellar continua are found to be markedly affected by abundance. A UV excess, delta(2600-V), is computed which is more sensitive by a factor of 10 to (Fe/H) than is delta(U-B). The relative strength of spectral lines in the mid-UV is not as strongly affected by abundance. Mid-UV spectra are much more sensitive to the temperature of the stellar population than to either metallicity or the dwarf/giant ratio. Mg II 2800 shows unexpected behavior, displaying no sensitivity to abundance for cool stars and a reversed sensitivity in FG dwarfs such that metal-poor stars have stronger Mg II strengths at the same temperature than more metal-rich stars.

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