J/AJ/144/35 Abundances of the eclipsing binary ZZ Boo (Kang+, 2012)
Chemical composition of the components of eclipsing binary star ZZ Bootis.
Kang Y.-W., Yushchenko A., Hong K., Kim S., Yushchenko V.
<Astron. J., 144, 35 (2012)>
=2012AJ....144...35K 2012AJ....144...35K
ADC_Keywords: Binaries, eclipsing ; Spectroscopy ; Abundances ;
Equivalent widths ; Effective temperatures
Keywords: accretion, accretion disks - binaries: general - stars: abundances -
stars: chemically peculiar - stars: individual (ZZ Boo)
Abstract:
We investigated ZZ Boo using a high-resolution (R=80000) spectrum
obtained at the BOES echelle spectrograph attached to a 1.8m telescope
at the Bohuynsan observatory in Korea. The atmospheric parameters of
the components were found using the published photometrical
observations and the abundance analysis of iron lines: the flux ratio
of the components FA/FB=1.12±0.15, the effective temperatures of
the components Teff=6860±20K and 6930±20K, the surface gravities
log g=3.72±0.10 and 3.84±0.10, the metallicities
[Fe/H]=-0.10±0.08 and -0.03±0.10, and the projected rotation
velocities vsin i=11.9±0.4km/s and 19.3±0.8km/s for the primary
and secondary components, respectively. The pointed errors are the
formal errors of the methods used; the systematic errors of the
temperatures, gravities, metallicities, and projected rotational
velocities can be as high as 250-300K, 0.3dex, 0.15dex, and 4km/s,
respectively. The abundances of 24 and 22 chemical elements were
determined in the atmospheres of the components. The abundance pattern
of the primary component shows the solar or slightly undersolar
abundances of all elements. CNO abundances are close to solar values.
The abundance pattern of this component resembles those of λ
Boo type stars. The abundances of light elements, except oxygen, in
the atmosphere of the secondary component are practically solar. The
abundances of barium and two detected lanthanides are close to the
solar values; the overabundance of oxygen is 0.9dex. The abundances of
two components are evidently different. The comparison of relative
abundances with the condensation temperatures and second ionization
potentials of the elements confirms the difference in abundance
patterns and allows discussion of the different accretion scenarios
for two components of this binary system.
Description:
The spectrum of ZZ Boo was obtained with the echelle spectrograph
(BOES) attached to the 1.8m telescope at the Bohyunsan Observatory at
the Korean Astronomy & Space Science Institute. The wavelength range
of the spectrum is 3800-9500Å. Spectral resolving power R=80000.
The star was observed at JDhel=2453369.407.
Objects:
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RA (2000) DE Designation(s)
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13 56 09.52 +25 55 07.4 ZZ Boo = HD 121648
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 51 125 Iron lines in the spectrum of ZZ Boo
table3.dat 108 158 Lines of other elements in the spectrum of
ZZ Boo: primary component
table4.dat 108 119 Lines of other elements in the spectrum of
ZZ Boo: secondary component
table5.dat 64 59 Mean abundances of chemical elements in the
atmospheres of components of ZZ Boo
refs.dat 130 23 References
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See also:
V/130 : Geneva-Copenhagen Survey of Solar neighbourhood III (Holmberg+, 2009)
VI/69 : Atomic Spectral Line List (Hirata+ 1995)
J/MNRAS/415/2238 : Abundances of TX UMa (Glazunova+, 2011)
J/A+A/511/A68 : Transitions of CrII (Gurell+, 2010)
J/ApJS/167/292 : Laboratory transition probabilities for Gd II
(Den Hartog+, 2006)
J/ApJ/645/613 : Abundances of HD 221170 (Ivans+, 2006)
J/PASP/118/636 : Alpha Per High res. spectral atlas at 3810-8100Å
(Lee+, 2006)
J/AJ/128/846 : VRI observations of CE Leonis (Kang+, 2004)
J/A+A/347/348 : Solar abundance of iron (Grevesse+, 1999)
J/A+AS/126/21 : Velocities and duplicity of F-type dwarfs (Nordstroem+ 1997)
J/A+A/281/161 : Radio emission from stars at 250GHz (Altenhoff+, 1994)
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 [4508/8825] Wavelength; in Å
16- 19 F4.1 10-13m EW-A ? Component A equivalent width; in mÅ
21- 24 F4.1 10-13m EW-B ? Component B equivalent width; in mÅ
26- 31 F6.3 [-] log(gf) [-4.2/0.645] Log of the oscillatory strength
33 I1 --- r_log(gf) Reference to log(gf), in refs.dat file
35- 39 F5.3 eV Elow Lower energy level Elow
41- 45 F5.3 [-] logN-A ? Component A abundance (where log N(H)=12)
47- 51 F5.3 [-] logN-B ? Component B abundance (where log N(H)=12)
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Byte-by-byte Description of file: table[34].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 [3856/8695] Wavelength; in Å
16- 21 F6.3 [-] log(gf) Log of the oscillatory strength
23- 24 I2 --- Ref [1/27]? Reference to log(gf), in refs.dat file
25 A1 --- f_Ref Flag on Ref (h) (1)
27- 32 F6.3 eV Elow Lower energy level Elow
34- 38 F5.3 [-] logN [0.8/9.7] ZZ Boo abundance (log N(H)=12)
40- 44 F5.3 [-] logNo [0.8/8.7]? Solar abundance
46- 51 F6.3 [Sun] DlogN [-0.573/0.993] Abundance relative to the Sun
53- 57 F5.3 --- Bl [0/1] ZZ Boo blending (1=clean line)
59- 63 F5.3 --- Bl0 [0/1]? Solar blending (1=clean line)
65- 69 F5.3 --- D [0/1] ZZ Boo Depth in synthetic spectra
71- 75 F5.3 --- Do [0/1]? Solar depth in synthetic spectra
77- 82 F6.3 --- e(T) ? ZZ Boo error in abundance for a change
in effective temperatures ±100K
84- 89 F6.3 --- e(g) ? ZZ Boo error in abundance for a cja,ge
in logg of +0.2dex
91- 95 F5.3 --- DC-best ZZ Boo depth in best combined synthetic
spectrum of the binary
97-102 F6.3 --- DC-0.5 ZZ Boo depth with under-abundance by 0.5dex
104-108 F5.3 --- DC+0.5 ZZ Boo depth with over-abundance by 0.5dex
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Note (1): the information about hyperfine or/and isotopic splitting was
used, wavelength and oscillator strength are for one of the components,
blending in synthetic spectra is also shown for one of the components.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 1 A1 --- Comp ZZ Boo component (A=primary component,
B=secondary component)
3- 4 I2 --- Z [6/64] Atomic number
6- 10 A5 --- Ion Investigated species identification
12- 13 I2 --- NL [1/76] Number of lines used
15- 19 F5.2 [Sun] Ab-best Best value abundance (ZZ Boo minus Solar)
20- 22 F3.2 [Sun] e_Ab-best ? error in Ab-best
24- 28 F5.2 [Sun] Ab+100K Abundance (ZZ Boo minus Solar) with effective
temperature shifted by +100K)
29- 31 F3.2 [Sun] e_Ab+100K ? error in Ab+100K
33- 37 F5.2 [Sun] Ab+0.2 Abundance (ZZ Boo minus Solar) with surface
gravity shifted by +0.2dex)
38- 40 F3.2 [Sun] e_Ab+0.2 ? error in Ab+0.2
42- 45 F4.2 [-] logN-best Best value of ZZ Boo absolute mean abundance
46- 48 F3.2 [-] e_logN-best ? error in logN-
50- 53 F4.2 [-] logN+100K Absolute mean abundance of ZZ Boo with
effective temperature shifted by +100K
54- 56 F3.2 [-] e_logN+100K ? error in logN+100K
58- 61 F4.2 [-] logN+0.2 Absolute mean abundance of ZZ Boo with
surface gravity shifted by +0.2cm/s2)
62- 64 F3.2 [-] e_logN+0.2 ? error in logN-logg
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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- 42 A19 --- Aut Authors's name
43-130 A88 --- Com Comments
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 20-Sep-2013