An Abundance Study in the Hg-Mn Star 46 Aquilae (HD 186122) with the SUBARU/HDS 1

• Published in: Publications of the Astronomical Society of Japan 2001-12, Vol.53 (6), p.1223-1230
• Main Authors: Sadakane, Kozo, Takada-Hidai, Masahide, Takeda, Yoichi, Ando, Hiroyasu, Aoki, Wako, Honda, Satoshi, Izumiura, Hideyuki, Kajino, Toshitaka, Kambe, Eiji, Kawanomoto, Satoshi, Noguchi, Kunio, Okita, Kiichi, Sato, Bun’ei, Watanabe, Etsuji
• Format: Article
• Language: English
• ISSN: 0004-6264; 2053-051X
• DOI: 10.1093/pasj/53.6.1223

A detailed abundance analysis has been carried out for the Hg-Mn star 46 Aql using high-resolution spectra in the visual region (5100–6400  ${Å}$ ) obtained with the High Dispersion Spectrograph of the Subaru Telescope. Our attention has been mainly focused on those elements which have not been analyzed previously. He, C, N, and O are underabundant, while Na shows the solar abundance. We have confirmed previously reported underabundances of Mg, Al, and Si, and have found an overabundances of P ( $+1.5\,\mathrm{dex}$ ) and Ti ( $+1.0 \,\mathrm{dex}$ ) and a significant underabundance of S ( $-1.8 \,\mathrm{dex}$ ). Fe is overabundant by $+0.8 \pm 0.1 \,\mathrm{dex}$ and a microturbulent velocity of $0.3 \,\mathrm{km} \,\mathrm{s}^{-1}$ was found from an analysis of the Fe ii lines. Among a few hundred unidentified absorption lines, we identified lines of As ii and Xe ii and a very large ( $+4.0 \,\mathrm{dex}$ ) overabundance of Xe is obtained. We have confirmed emission lines of Mn ii and Ti ii near 6100  ${Å}$ , while those of Cr ii cannot have been seen.