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 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:
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RA (2000) DE Designation(s)
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23 29 28.8 +30 25 58 HD 221170 = HIP 115949
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File Summary:
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FileName Lrecl Records Explanations
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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
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): Notes as follows:
a = loggf from Ivarsson et al. (2003A&A...409.1141I 2003A&A...409.1141I)
b = loggf from Nillson et al. (2002A&A...382..368N 2002A&A...382..368N) and
Nillson et al. (2002A&A...381.1090N 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)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 30-Jun-2006