Volume 420, Number 2, June III 2004
|Page(s)||673 - 681|
|Published online||28 May 2004|
Rakutou High School, Anshu, Yamashina-ku, Kyoto 607-8017, Japan
2 Astronomical Institute, Osaka Kyoiku University, Asahigaoka, Kashiwara, Osaka 582-8582, Japan
3 Osaka Science Museum, Nakanoshima, Kita-ku, Osaka 530-0005, Japan
4 National Astronomical Observatory, Osawa, Mitaka, Tokyo 181-8588, Japan
5 European Southern Observatory, Casilla 19001, Santiago 19, Chile
Corresponding author: M. Nishimura, firstname.lastname@example.org
Accepted: 23 February 2004
A spectrum synthesis analysis for photospheric lines in the magnetic B star HR 5049 is presented, based on a high quality spectrogram obtained with the EMMI spectrograph attached to the NTT at ESO. It is found that light elements such as He, C and O are under-abundant. One of the most notable features is the deficiency of He by more than -2.0 dex. Co and Cl are over-abundant by +3.5 dex and +1.9 dex, respectively. Other iron peak elements are over-abundant ranging from +0.47 dex () to +1.94 dex (). For rare earth elements, the lines of once-ionized species are generally weak, while the third spectra (especially those of Pr and Nd) are very prominent. Although rare earth elements show significant over-abundances ranging from +3.0 dex to as large as +4.0 dex, Ba has the solar abundance. The Nd-Pr abundance difference, which shows an apparent decreasing trend with increasing effective temperature among CP stars, is found to be unusually small in HR 5049.
Key words: stars: abundances / stars: chemically peculiar / stars: individual: HR 5049
Based on observations collected at the La Silla Observatory, ESO (Chile) with the New Technology Telescope (NTT).
© ESO, 2004
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