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J/A+A/430/255       Abundances of HD221170               (Yushchenko+, 2005)

Thorium-rich halo star HD 221170: Further evidence against the universality of the r-process. Yushchenko A., Gopka V., Goriely S., Musaev F., Shavrina A., Kim C., Woon Kang Y., Kuznietsova J., Yushchenko V. <Astron. Astrophys., 430, 255-262 (2005)> =2005A&A...430..255Y
ADC_Keywords: Stars, variable ; Abundances ; Spectroscopy Keywords: line: identification - stars: abundances - stars: atmospheres - stars: evolution - stars: individual: HD 221170 - nuclear reactions, nucleosynthesis, abundances Abstract: We report the abundance determination in the atmosphere of the bright halo star HD 221170. The spectra were taken with the Terskol Observatory's 2.0-m telescope with a resolution R=45000 and signal-to-noise ratio up to 250 in the wavelength region 3638-10275Å. The abundances of 43 chemical elements were determined with the method of spectrum synthesis. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 23 29 28.8 +30 25 58 HD 221170 = HIP 115949 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 38 251 Iron lines in the spectrum of HD 221170 table2.dat 94 617 Lines of other elements in the spectrum of HD 221170
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 F8.3 0.1nm lambda Wavelength 10- 14 A5 --- Ion Ion 16- 20 F5.1 0.1pm EW Equivalent width 22- 26 F5.2 [-] loggf Oscillator strength 28- 32 F5.3 eV Elow Energy of lower level 34- 38 F5.3 --- logN Abundance, in logN(H)=12 scale
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 5 F5.2 --- Ion Ion number (e.g. 26.00 = Fe I) 7- 14 F8.3 0.1nm lambda Wavelength 16- 22 F7.3 [-] loggf Oscillator strength 23 A1 --- n_loggf [ab] Note on loggf (1) 25- 29 F5.3 eV Elow Energy of lower level 31 A1 --- l_Abun Limit flag on DlogN 32- 37 F6.3 [Sun] Abun Abundance of ion (relative to Sun, log scale) 39 A1 --- l_logN Limit flag on logN 40- 45 F6.3 [-] logN HD 221170 abundance (in logN(H)=12 scale)(2) 47- 52 F6.3 [-] logNS ?=- Sun abundance (in logN(H)=12 scale) 54- 58 F5.3 --- Blend ?=- HD 221170 level of blending (1=clean line) 59 A1 --- n_Blend [h] h for hfs (unexplained) 61- 65 F5.3 --- BlendS ?=- Sun level of blending (1=clean line) 66 A1 --- n_BlendS [h] h for hfs (unexplained) 68- 72 F5.3 --- Depth ?=- HD 221170 depth in synthetic spectra (2) 73 A1 --- n_Depth [h] h for hfs (unexplained) 75- 79 F5.3 --- DepthS ?=- Sun depth in synthetic spectra 80 A1 --- n_DepthS [h] h for hfs (unexplained) 82- 87 F6.3 [Sun] dAbG ?=- Abundance change with logg (+0.2) 89- 94 F6.3 [Sun] dAbT ?=- Abundance change with Teff (+100K)
Note (1): Notes as follows: a = loggf from Ivarsson et al. (2003A&A...409.1141I) b = loggf from Nillson et al. (2002A&A...382..368N) and Nillson et al. (2002A&A...381.1090N) Note (2): Calculated with two different atmosphere models, namely for a surface gravity increased by 0.2dex, and for an effective temperature increased by 100K (Teff=4475K, logg=1.2 and Teff=4575K, logg=1.0)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 30-Jun-2006
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