Issue |
A&A
Volume 420, Number 2, June III 2004
|
|
---|---|---|
Page(s) | 673 - 681 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361:20035651 | |
Published online | 28 May 2004 |
Chemical composition of the magnetic B star HR 5049 *,**
1
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, mnisimura@kcat.zaq.ne.jp
Received:
10
November
2003
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
© ESO, 2004
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