J/AJ/134/926 Chemical composition of V2314 Oph (Kim+, 2007)
Chemical composition and differential time-series CCD photometry of
V2314 Ophiuchi: a new λ Bootis-type star.
Kim C., Yushchenko A.V., Gopka V.F., Dorokhova T.N., Musaev F.A.,
Kim S.-L., Jeon Y.-B., Ibrahimov M., Tarasov A.E.
<Astron. J., 134, 926-933 (2007)>
=2007AJ....134..926K 2007AJ....134..926K
ADC_Keywords: Stars, variable ; Spectroscopy ; Abundances
Keywords: stars: abundances - stars: oscillations -
stars: individual
(V2314 Ophiuchi, SX Phoenicis, delta Scuti, lambda Bootis)
Abstract:
We investigated V2314 Oph using high-resolution (R=45000) spectral
observations. The atmospheric parameters were determined using
iron-line abundance analysis. We derived a mean effective temperature
of Teff=7510K, mean surface gravity of logg=3.30, metallicity of
[Fe/H]=-0.59, and rotation velocity of vsini=38km/s. The abundances of
19 chemical elements were determined.
Description:
Seven spectra of V2314 Oph were obtained during three nights in 2002
using a coude-echelle spectrometer mounted on the 2m Zeiss telescope
at the Peak Terskol Observatory located near Mount Elbrus (Northern
Caucasus, Russia), 3124m above sea level.
Objects:
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RA (2000) DE Designation(s)
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17 44 03.6 +06 03 43 V2314 Oph = V* V2314 Oph
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 36 168 Iron lines in the spectrum of V2314 Oph
table4.dat 85 111 Lines of other elements in the spectrum of V2314 Oph
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See also:
B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2009)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm Wave Wavelength in Angstroms
10- 14 A5 --- Ion Iron species
16- 18 I3 0.1pm EW Equivalent width in milli-Angstroms
20- 24 F5.2 [-] log(gf) Log of the oscillator strength
26- 30 F5.3 eV Elow Energy of the low level
32- 36 F5.3 [-] logN Log of the iron number abundance (logH=12)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 5 F5.2 --- Ion Ion identification code (e.g. FeI = 26.00)
7- 14 F8.3 0.1nm Wave Wavelength in Angstroms
16- 21 F6.3 [-] log(gf) Log of the oscillator strength
23- 28 F6.3 eV Elow Excitation energy
30- 35 F6.3 [-] DlogN Log of abundance difference from solar (2)
37- 41 F5.3 [-] logN Log of V2314 Oph element abundance
43- 47 F5.3 [-] logNSun ? Log of solar element abundance (2)
49- 53 F5.3 --- bld [0,1] Level of synthetic spectrum line
blending in V2314 Oph (3)
55- 59 F5.3 --- bldSun [0,1]? Level of synthetic spectrum line
blending in Sun (3)
61- 65 F5.3 --- Depth [0,1] Synthetic spectrum line depth
in V2314 Oph
67- 71 F5.3 --- DepthSun [0,1]? Synthetic spectrum line depth in Sun
73- 78 F6.3 [-] dlog(gf) Change of log of the abundance for atmosphere
model with log(gf) shifted by -0.2dex
80- 85 F6.3 [-] dTeff Change of log of the abundance for atmosphere
model with Teff shifted by +100K
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Note (2): If the value of solar abundance in the column marked as 'logNSun'
is NULL the abundance from Grevesse & Sauval (1998,
Space Sci. Rev., 85, 161) is used.
Note (3): where 1.0 = clean line, and
0.0 = strongly blended line
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 03-Oct-2009