J/PASP/124/401 Chemical composition of BE Lyn (Kim+, 2012)
Chemical composition and photometry of BE Lyncis.
Kim C., Yushchenko A.V., Kim S.-L., Jeon Y.-B., Kim C.-H.
<Publ. Astron. Soc. Pac., 124, 401-410 (2012)>
=2012PASP..124..401K 2012PASP..124..401K
ADC_Keywords: Stars, variable ; Abundances
Keywords: Stars
Abstract:
High-resolution spectroscopic observation was carried out to find the
chemical composition of BE Lyn. The abundances of 25 chemical elements
from carbon to neodymium were found. The deficiency of iron appeared
to be equal to {DELTA}logN(Fe)=-0.26±0.08 with respect to the solar
metallicity, and the abundances of other elements were mainly
undersolar. Only nitrogen, sodium, aluminium, and sulfur showed
overabundances near 0.2-0.3dex. The abundance pattern showed no
clear signs of accretion or mass transfer events. It is not possible
to exclude the classification of BE Lyn as a SX Phe-type star with
slightly undersolar abundances of chemical elements. In addition, new
differential time-series observations of BE Lyn were secured using V
filters, and seven new times of light maximum were identified. We
collected 162 times of light maximum from the literature, unpublished
data, and an open database, and we proceeded to investigate the
pulsational properties of BE Lyn. All five harmonic frequencies were
identified using the Fourier decomposition method.
Description:
To estimate the metallicity, high-resolution spectra of BE Lyn were
obtained using a Bohyunsan echelle spectrograph (BOES) fed by the 1.8m
telescope of the Bohyunsan Optical Astronomy Observatory in Korea. The
spectra were recorded during one night: 2009 January 3. The resolving
power of the spectra is R=45000, the signal-to-noise ratio (S/N) is
near 100 in the red spectral region, and the wavelength coverage is
from 3800 to 9600Å.
Objects:
-----------------------------------------------
RA (2000) DE Designation(s)
-----------------------------------------------
09 18 17.18 +46 09 11.3 BE Lyn = HD 79889
-----------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 37 147 Iron Lines in Spectrum of BE Lyn
table2.dat 116 242 Lines of chemical elements in spectrum of
BE Lyn (except iron)
refs.dat 127 22 References
table3.dat 89 34 Mean abundances of chemical elements in
atmosphere of BE Lyn
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.4 0.1nm lambda Wavelength
11- 15 A5 --- Ion Ion (Fe I or Fe II)
17- 21 F5.2 [-] loggf Oscillator strength
23- 27 F5.3 eV Elow Energy of low level
29- 31 I3 0.1pm EW Equivalent width (in mÅ)
33- 37 F5.3 [-] logN Iron abundance (in the scale of logN(H)=12)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 F5.2 --- Ion Ion numerial code (FeI=26.00)
7- 14 F8.3 0.1nm lambda Wavelength
16- 21 F6.3 [-] loggf Oscillator strength
23- 24 I2 --- r_loggf Reference for loggf, in refs.dat file
26- 31 F6.3 eV Elow Excitation potential
33- 38 F6.3 [-] DlogN Differential abundance, Be Lyn - Sun
(in the scale of logN(H)=12)
40- 44 F5.3 [-] logN* BE Lyn abundance (in the scale of logN(H)=12)
46- 50 F5.3 [-] logNS ?=- Sun abundance (in the scale of logN(H)=12)
52- 56 F5.3 --- Bl* ?=- Be Lyn level of blending of the line in
the synthetic spectra
(1 = clean line, 0.0 = strong blended line)
57 A1 --- n_Bl* [h] h for hfs: hyperfine splitting
59- 63 F5.3 --- BlS ?=- Sun level blending of the line in the
synthetic spectra
(1 = clean line, 0.0 = strong blended line)
64 A1 --- n_BlS [h] h for hfs: hyperfine splitting
66- 70 F5.3 --- D* BE Lyn depth of the line in synthetic spectra
72- 76 F5.3 --- DS ?=- Sun depth of the line in synthetic spectra
78- 83 F6.3 [-] dA(T) Correction for abundance, by an effective
temperature decrease of 200K
85- 90 F6.3 [-] dA(g) Correction for abundance, by a gravity
increase of 0.3dex
92- 97 F6.3 [-] dA(vt) Correction for abundance, by a
microturbulent velocity increase of 0.5km/s
99-103 F5.3 --- D Depth of the line in convoluted synthetic
spectra
105-110 F6.3 --- dD1 Correction to the best depth of the line in
the synthetic spectrum found by changing the
abundance of the investigated chemical
element by -0.5dex
112-116 F5.3 --- dD2 Correction to the best depth of the line in
the synthetic spectrum found by changing the
abundance of the investigated chemical
element by +0.5dex
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Ref Reference number
4-127 A124 --- Com Reference
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Z Atomic number
4- 9 A6 --- Ion Ion
11- 13 I3 --- n Number of line used
15- 19 F5.2 [-] DlogN Relative abundance in BL Lyn atmosphere,
best value
21- 23 F3.2 [-] e_DlogN ? rms uncertainty on DlogN
25- 29 F5.2 [-] DlogN1 Relative abundance in BL Lyn atmosphere,
effective temperature increased by 100K
31- 33 F3.2 [-] e_DlogN1 ? rms uncertainty on DlogN1
35- 39 F5.2 [-] DlogN2 Relative abundance in BL Lyn atmosphere,
surface gravity decreased by 0.3dex
41- 43 F3.2 [-] e_DlogN2 ? rms uncertainty on DlogN2
45- 49 F5.2 [-] DlogN3 Relative abundance in BL Lyn atmosphere,
microturbulent velocity increased by 0.5km/s
51- 53 F3.2 [-] e_DlogN3 ? rms uncertainty on DlogN3
55- 58 F4.2 [-] logN Absolute abundance in BL Lyn atmosphere,
best value
60- 62 F3.2 [-] e_logN ? rms uncertainty on logN
64- 67 F4.2 [-] logN1 Absolute abundance in BL Lyn atmosphere,
effective temperature increased by 100K
69- 71 F3.2 [-] e_logN1 ? rms uncertainty on logN1
73- 76 F4.2 [-] logN2 Absolute abundance in BL Lyn atmosphere,
surface gravity decreased by 0.3dex
78- 80 F3.2 [-] e_logN2 ? rms uncertainty on logN2
82- 85 F4.2 [-] logN3 Absolute abundance in BL Lyn atmosphere,
microturbulent velocity increased by 0.5km/s
87- 89 F3.2 [-] e_logN3 ? rms uncertainty on logN3
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 21-Mar-2013