Elemental abundance analyses with DAO spectrograms

XXIX. The mercury-manganese stars 53 Tau, β Tau, γ Crv, and υ Her

¹ Department of Physics, The Citadel, 171 Moultrie Street, Charleston, SC 29409, USA e-mail: adelmans@citadel.edu
² Guest Investigator, Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 W. Saanich Road, Victoria V8X 4M6 Canada
³ İstanbul University, Department of Astronomy and Space Sciences, 34119 University, İstanbul, Turkey
⁴ Department of Physics, Brandon University, Brandon, MB R7A 6A9 Canada
⁵ İstanbul Kültür University, Department of Physics, Faculty of Science & Letters, E5 Karayolu Üzeri, 34510, Şirinevler, İstanbul, Turkey

Received: 6 June 2005
Accepted: 4 October 2005

Abstract

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 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.