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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
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 --------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 40 172 Analyses of individual atomic lines table2.tex 104 488 LaTeX version of table2
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
Bytes Format Units Label Explanations
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)
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 HH = Hirata, & Horaguchi, T. 1995, Cat. VI/69 KX = Kurucz, R.L. 2001, http://kurucz.harvard.edu/ LB = Lawler et al., 2001ApJ...556..452L LW = Lawler et al., 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.
Acknowledgements: Masayoshi Nishimura
(End) Patricia Bauer [CDS] 07-Jun-2004
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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