Elemental abundance analyses with DAO spectrograms. XXIX. The mercury-manganese stars 53 Tau, β Tau, γ Crv, and υ Her

Details Elemental abundance analyses with DAO spectrograms. XXIX. The mercury-manganese stars 53 Tau, β Tau, γ Crv, and υ Her Elemental abundance analyses with DAO spectrograms. XXIX. The mercury-manganese stars 53 Tau, β Tau, γ Crv, and υ Her

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...447..685a&link_type=abstract

Astronomy and Astrophysics, Volume 447, Issue 2, February IV 2006, pp.685-690

Astronomy and Astrophysics

Astrophysics

11

Stars: Abundances, Stars: Individual: 53 Tau, Stars: Individual: Β Tau, Stars: Individual: Γ Crv, Stars: Individual: Υ Her, Stars: Chemically Peculiar

Scientific paper

We performed elemental abundances analyses of the mercury-manganese (HgMn) stars 53 Tau, β Tau, and γ Crv consistent with previous studies of similar stars in this series. The derived v sin i values for the last two stars are 59 and 32 km s-1, respectively, both of which are greater than those of HgMn stars previously studied. For 53 Tau this analysis using selected wavelength regions replaces one performed with coadded photographic spectra. A stricter upper limit is placed on any Hg II λ3984 line. The abundances of β Tau are usually greater than those of γ Crv. But the later star has a Hg II λ3984 line which the former lacks. Our analysis of υ Her, which was performed with spectrograms obtained with CCD detectors, is extended by using additional spectrograms to increase the range of wavelengths covered longward of λ4800. Minor changes in the derived abundances result.

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