J/A+A/420/673 Elemental abundances of CP2 star HR 5049 (Nishimura+, 2004)
Chemical composition of the magnetic B star HR 5049.
Nishimura M., Sadakane K., Kato K., Takeda Y., Mathys G.
<Astron. Astrophys. 420, 673 (2004)>
=2004A&A...420..673N 2004A&A...420..673N
ADC_Keywords: Stars, Bp ; Abundances, peculiar
Keywords: stars: abundances - stars: chemically peculiar -
stars: individual: HR 5049
Abstract:
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
-2.0dex. Co and Cl are over-abundant by +3.5dex and +1.9dex,
respectively. Other iron peak elements are over-abundant ranging from
+0.47dex (Ti II) to +1.94 dex (Cr I). 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
+3.0dex to as large as +4.0dex, 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.
Description:
We use a CCD spectrogram ranging from λ4070Å to
λ6700Å which was obtained with the ESO New Technology
Telescope (NTT) and the ESO Multi-Mode Instrument (EMMI) in the
cross-dispersed echelle mode.
The elemental abundances for individual lines of HR 5049 are
determined by spectral synthesis.
Objects:
---------------------------------------------
RA (2000) DE Designation(s)
---------------------------------------------
13 25 50.3 -70 37 38 HR 5049 = HD 116458
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 40 172 Analyses of individual atomic lines
table2.tex 104 488 LaTeX version of table2
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See also:
J/A+A/407/631 : Catalogue of stellar effective magnetic fields (Bychkov+ 2003)
J/A+AS/118/231 : Velocities + rotation of CP stars (Levato+, 1996)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Ion Ion designation
8- 14 F7.2 0.1nm lambda Wavelength
16- 20 F5.2 eV Chi ? Excitation potential
22- 26 F5.2 --- loggf ? Oscillator strength
28- 29 A2 --- r_loggf Reference for loggf (1)
31- 32 A2 --- l_logN/H [≤ ] Limit flag on logN/H
33- 36 F4.2 [---] logN/H ? Elemental abundance logN/H
38- 40 A3 ---- Remark Remarks (2)
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Note (1): gf-value references:
B = Biemont et al., 2002, http://www.umh.ac.be/~astro/dream.shtml
BF = Biemont et al., 1989A&A...209..391B 1989A&A...209..391B
HH = Hirata, & Horaguchi, T. 1995, Cat. VI/69
KX = Kurucz, R.L. 2001, http://kurucz.harvard.edu/
LB = Lawler et al., 2001ApJ...556..452L 2001ApJ...556..452L
LW = Lawler et al., 2001ApJ...563.1075L 2001ApJ...563.1075L
MR = Mashonkina et al., 2002, Cat. J/PAZh/28/41
NI = NIST, 2000, http://physics.nist.gov/PhysRefData/contents-atomic.html
RU = Raasen & Uylings, 2000, http://www.science.uva.nl/pub/orth/iron/FeII.E1
Note (2): Remarks:
HFS = the abundances determined by adopting the HFS data taken from
Kurucz, 2001, http://kurucz.harvard.edu/
C* = the abundance determined using several lines of the same numbers (*)
in reference.
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Acknowledgements: Masayoshi Nishimura
(End) Patricia Bauer [CDS] 07-Jun-2004