J/AJ/145/167 Abundances of LX Per (Kang+, 2013)
Signs of accretion in the abundance patterns of the components of the
RS CVn-type eclipsing binary star LX Persei.
Kang Y.-W., Yushchenko A.V., Hong K., Guinan E.F., Gopka V.F.
<Astron. J., 145, 167 (2013)>
=2013AJ....145..167K 2013AJ....145..167K
ADC_Keywords: Binaries, eclipsing ; Abundances ; Equivalent widths
Keywords: accretion, accretion disks - binaries: general - stars: abundances -
stars: chemically peculiar - stars: chromospheres - starspots
Abstract:
We present spectroscopic observations of LX Per carried out using the
Korean Bohyunsan Observatory Echelle Spectrograph (BOES) with spectral
resolving power R=80000. The spectrograph was attached to the 1.8m
telescope. The fit of synthetic spectra to the observed spectrum of
the system allowed us to find the component parameters and the
abundances of chemical elements in the atmospheres of the components.
The strong CaII H&K emissions are confirmed; we also found emission
lines in the CaII reversals' triplet absorptions at the wavelengths of
8498, 8542, and 8662Å in the spectrum of the cooler component of LX
Per. A unique photometric solution using the distorted light curves of
three different epochs was made. The spot model light curves were
fitted to the 1981, 1982, and 1983 observations successfully by
adjusting only spot parameters. We could infer that the variation of
spot location and size was the main reason for the changing shape of
light curves. The main feature of the abundance patterns of both
components was the apparent deficiency of heavy (Z>30) elements. Only
elements with strong lines, namely Y and Ba, were detected.
Correlations of relative abundances of chemical elements with
condensation temperatures and second ionization potentials of these
elements, which can be explained by the accretion of dust and gas,
were found.
Description:
Spectroscopic observations were carried out with the Bohyunsan
Observatory Echelle Spectrograph (BOES) attached to the 1.8m telescope
at the Bohyunsan Observatory of the Korea Astronomy and Space Science
Institute (KASI). One spectrum of LX Per was obtained at JD
2453368.9545 (mid-exposure) with a wavelength range of 3800-9500Å
and a spectral resolving power R=80000. It was permitted to reach a
signal-to-noise ratio (S/N) of 100-110 at wavelengths 5500-6000Å,
an S/N of 50 at 4150-9500Å, and an S/N of 20 at 3800Å.
Objects:
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RA (ICRS) DE Designation(s)
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03 13 22.37 +48 06 31.3 LX Persei = HIP 15003
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 53 107 Iron lines in the spectrum of LX Per
table5.dat 89 110 Lines of chemical elements (except iron) in the
spectrum of the hotter component of LX Per
table6.dat 89 123 Lines of chemical elements (except iron) in the
spectrum of the cooler component of LX Per
table7.dat 70 53 Mean abundances of chemical elements in the
atmosphere of LX Per
refs.dat 118 15 References
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See also:
VI/69 : Atomic Spectral Line List (Hirata+ 1995)
J/AJ/144/35 : Abundances of the eclipsing binary ZZ Boo (Kang+, 2012)
J/ApJ/645/613 : Abundances of HD 221170 (Ivans+, 2006)
J/PASP/118/636 : al. Per High res. spectral atlas at 3810-8100Å (Lee+, 2006)
J/A+A/347/348 : Solar abundance of iron (Grevesse+, 1999)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Ion Iron line identifier (Fe I or Fe II)
7- 14 F8.3 0.1nm lambda [4515/8946] Wavelength; in Å
16- 21 F6.3 [-] loggf Log of the oscillator strength
23- 24 A2 --- r_loggf Reference for loggf; in refs.dat file
26- 30 F5.3 eV Elow Lower excitation energy level
32- 35 F4.1 0.1pm EWh ? Equivalent width of hot component (mÅ)
37- 41 F5.1 0.1pm EWc ? Equivalent width of cool component (mÅ)
43- 47 F5.3 [-] logNh ? Hot component abundance (logN(H)=12)
49- 53 F5.3 [-] logNc ? Cool component abundance (logN(H)=12)
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Byte-by-byte Description of file: table[56].dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Ion Elemental line identification
7- 14 F8.3 0.1nm lambda [4497/9238] Line wavelength; in Å
16- 21 F6.3 [-] loggf Log of the oscillator strength
22 A1 --- f_loggf [h] Flag on loggf (h) (1)
24- 25 A2 --- r_loggf Reference for loggf; in refs.dat file
27- 32 F6.3 eV Elow Excitation energy of lower level
34- 38 F5.3 [-] logN Derived abundance in LX Per (H=12)
40- 44 F5.3 [-] logNo ? Derived abundance in the Sun (H=12)
46- 51 F6.3 [Sun] Abun LX Per abundance relative to the Sun
53- 57 F5.3 --- Bl [0/1] Blending in LX Per (1=clean line)
59- 63 F5.3 --- Blo [0/1]? Blending in the Sun (1=clean line)
65- 69 F5.3 --- D [0/1] LX Per depth in synthetic spectrum
71- 75 F5.3 --- Do [0/1]? Solar depth in synthetic spectrum
77- 82 F6.3 [-] e(g) LX Per error in abundance for a change in logg
of +0.2dex
84- 89 F6.3 [-] e(T) LX Per error in abundance for a change in
effective temperature of +100K
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Note (1): Isotopic splitting and hyperfine structure of the lines were taken
into account for Li, Sc, V, Mn, Co, Cu, and Ba.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1 A1 --- C [ch] Component (h=hotter, c=cooler)
3- 4 I2 --- Z [3/56]? Atomic number
6- 10 A5 --- Ion Name of ion
12- 13 I2 --- NL [1/72] Number of spectral lines used
15- 19 F5.2 [Sun] Abest Best value mean abundance (LX Per minus Solar)
21- 23 F3.2 [Sun] e_Abest ? Uncertainty in Ab-best
25- 29 F5.2 [Sun] Ag+0.2 Mean abundance (LX Per minus Solar) with
surface gravity shifted by +0.2cm/s2
31- 33 F3.2 [Sun] e_Ag+0.2 ? Uncertainty in Ag+0.2
35- 39 F5.2 [Sun] A+100K Mean abundance (LX Per minus Solar) with
effective temperature altered by +100K
41- 43 F3.2 [Sun] e_A+100K ? Uncertainty in A+100K
45- 48 F4.2 [-] Nbest Best value of LX Per absolute mean abundance
log(N/H)+12
50- 52 F3.2 [-] e_Nbest ? Uncertainty in N-best
54- 57 F4.2 [-] Ng+0.2 Absolute mean abundance of LX Per with surface
gravity shifted by +0.2cm/s2
59- 61 F3.2 [-] e_Ng+0.2 ? Uncertainty in N+0.2
63- 66 F4.2 [-] N+100K Absolute mean abundance (log(N/H)+12) of LX Per
with effective temperature altered by +100K
68- 70 F3.2 [-] e_N+100K ? Uncertainty in N+100K
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref [1/27] Reference number
4- 22 A19 --- BibCode Bibliographic code
24- 44 A21 --- Aut Authors's name
46-118 A73 --- Com Comments
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 02-Jun-2014