TY - JOUR
T1 - An abundance study in the Hg-Mn star 46 Aquilae (HD 186122) with the SUBARU/HDS
AU - Sadakane, Kozo
AU - Takada-Hidai, Masahide
AU - Takeda, Yoichi
AU - Ando, Hiroyasu
AU - Aoki, Wako
AU - Honda, Satoshi
AU - Izumiura, Hideyuki
AU - Kajino, Toshitaka
AU - Kambe, Eiji
AU - Kawanomoto, Satoshi
AU - Noguchi, Kunio
AU - Okita, Kiichi
AU - Sato, Bun'ei
AU - Watanabe, Etsuji
PY - 2001
Y1 - 2001
N2 - 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 (+1.5dex) and Ti (+ 1.0dex) and a significant underabundance of S (-1.8dex). Fe is overabundant by +0.8±0.1 dex and a microturbulent velocity of 0.3kms-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 (+4.0dex) 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.
AB - 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 (+1.5dex) and Ti (+ 1.0dex) and a significant underabundance of S (-1.8dex). Fe is overabundant by +0.8±0.1 dex and a microturbulent velocity of 0.3kms-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 (+4.0dex) 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.
KW - Stars: Abundances
KW - Stars: Chemically peculiar
KW - Stars: Individual (46 Aquilae = HD 186122)
UR - https://www.scopus.com/pages/publications/0035528391
U2 - 10.1093/pasj/53.6.1223
DO - 10.1093/pasj/53.6.1223
M3 - 文章
AN - SCOPUS:0035528391
SN - 0004-6264
VL - 53
SP - 1223
EP - 1230
JO - Publications of the Astronomical Society of Japan
JF - Publications of the Astronomical Society of Japan
IS - 6
ER -