Other
Scientific paper
Jun 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.9304p&link_type=abstract
American Astronomical Society, 200th AAS Meeting, #93.04; Bulletin of the American Astronomical Society, Vol. 34, p.954
Other
Scientific paper
AV 304 is a sharp-lined B0.5V star in the Small Magellanic Cloud. The abundances of Ti, Cr, Mn, and Fe have been determined using spectra obtained with HST/STIS and the Kurucz LTE model atmosphere/spectrum synthesis codes ATLAS9/SYNTHE. A model of Teff = 26,500 K, log g = 4.0, and [M/H] = -0.5 was adopted based upon a least squares fit to IUE LORES data and the UBV magnitudes for the star. Other input parameters used included Vturb = 1 km s-1 (from the continuum fit), v sin i = 20 km s-1, and instrumental broadening parameters of 12,000 and 11,000 corresponding to resolving powers for the STIS/G140M & 230M gratings. Mean abundances, [X/H]sun, of -0.72+/-0.41, -0.97+/-0.06, -1.04+/-0.14, and -0.61+/-0.30 were found for Ti, Cr, Mn, and Fe from 4, 3, 2, and 65 lines of Ti 3, Cr 3, Mn 3, and Fe 3, respectively. The mean Fe abundance agrees well with that determined from lines in the ISM and A supergiants. The underabundance of the α element Ti is similar to that of Fe, but Cr and Mn appear to have lower abundances than the mean values from ISM lines. It would be worthwhile to analyze additional UV lines of Cr and Mn that were not contained in this database. The chemical evolution in the region of the SMC where AV 304 resides does not seem to be significantly different from the typical one in this galaxy. This project was partially supported by GO-06709-95A from the Space Telescope Science Institute.
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