Open AccessAn elemental abundance analysis of the mercury manganese star HD 29647
Author(s) -
Adelman S.J.,
Snow T.P.,
Wood E.L.,
Evans I.I.,
Sneden C.,
Ehrenfreund P.,
Foing B.H.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04936.x
Subject(s) - physics , astrophysics , stars , astronomy , mercury (programming language) , observatory , spectral line , line (geometry) , geometry , mathematics , computer science , programming language
The sharp‐lined mercury manganese (HgMn) star HD 29647, which is located behind the outer envelope of the Taurus Molecular Cloud 1, is of interest for both its stellar properties and its utility as a probe of interstellar gas and dust along its line of sight. In this paper we review the properties of the star, summarize its line identifications and present an abundance analysis based on spectrograms obtained at the McDonald Observatory and the Observatoire de Haute‐Provence. This star has elemental abundances similar to those of other HgMn stars except that its He/H ratio is closer to solar, possibly indicating a young age, and that it, like HR 7775, is overabundant in selected elements including the rare earths. The stellar radial velocity, unfortunately, closely matches that of the foreground cloud.