The Chemical Compositions of the 2 New Hgmn Stars HD 30085 and HD
Draft version August 15, 2019 A Preprint typeset using L TEX style AASTeX6 v. 1.0 THE CHEMICAL COMPOSITIONS OF THE 2 NEW HGMN STARS HD 30085 AND HD 30963. COMPARISON TO χ LUPI A, ν CAP AND HD 174567 R. Monier1 LESIA, UMR 8109, Observatoire de Paris et Universit´ePierre et Marie Curie Sorbonne Universit´es, place J. Janssen, Meudon, France. E.Griffin2 Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada M. Gebran3 Department of Physics and Astronomy, Notre Dame University-Louaize, PO Box 72, Zouk Mikael, Lebanon. T. Kılıc¸oglu˘ 4 Department of Astronomy and Space Sciences, Faculty of Science, Ankara University, 06100, Turkey. T.Merle5 Institut d’Astronomie et d’Astrophysique, Universit´eLibre de Bruxelles, CP 226, Boulevard du Triomphe, 1050 Brussels, Belgium F. Royer6 GEPI, Observatoire de Paris, place J. Janssen, Meudon, France. ABSTRACT We report on a detailed abundance study of the fairly bright slow rotators HD 30085 (A0 IV), HD 30963 (B9 III) and HD 174567 (A0 V), hitherto reported as normal stars and the sharp-lined χ Lupi A (B9 IV HgMn). In the spectra of HD 30085, HD 30963, the Hg II line at 3984 A˚ line is conspicuous and numerous lines of silicon, manganese, chromium, titanium, iron, strontium, yttrium and zirconium appear to be strong absorbers. A comparison of the mean spectra of HD 30085 and HD 30963 with a grid of synthetic spectra for selected unblended lines having reliable updated atomic data reveals large overabundances of phosphorus, titanium, chromium, manganese, strontium, yttrium, and zirconium, barium, platinum and mercury and underabundances of helium, magnesium, scandium, arXiv:1908.05023v1 [astro-ph.SR] 14 Aug 2019 nickel.
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