J/AJ/164/149 Optical spectra of V367 Cygni with McKellar coude (Davidge, 2022)
Coaxing the Eclipsing Binary V367 Cygni out of Its Shell.
Davidge T.J.
<Astron. J., 164, 149 (2022)>
=2022AJ....164..149D 2022AJ....164..149D
ADC_Keywords: Stars, double and multiple; Spectra, optical
Keywords: Close binary stars ; Semi-detached binary stars
Abstract:
Spectra that cover 0.63-0.69µm with a spectral resolution ∼17000
are presented of the W Serpentis system V367-Cygni. Absorption lines
of FeII and SiII that form in a circumsystem shell are prominent
features, and the depths of these are stable with time, suggesting
that the shell is smoothly distributed and well mixed. Further
evidence of uniformity comes from modest radial velocity variations
measured in the deepest parts of the shell lines. It is suggested that
motions previously attributed to rotation of the shell are instead
artifacts of contamination from the donor star spectrum. A donor star
spectrum is extracted that is consistent with that of an early to
mid-A giant. The depths of metallic lines in the donor spectrum vary
with orbital phase, suggesting that spot activity covers a large
fraction of the surface of that star. A spectrum of the accretion disk
that surrounds the second star is also extracted, and similarities are
noted with the emission spectra of Herbig Ae/Be stars. In addition to
variations with orbital phase, Hα changes with time over
timescales of no more than two orbits. A tentative detection of HeI
6678 emission is made near primary minimum, but not at other phases.
Finally, projected emission from hot dust in and around V367-Cyg is
more or less symmetric and extends over 28", or 0.09pc at the distance
of the system; V367-Cyg is thus expelling matter into a large volume
of the surrounding space.
Description:
The spectra were recorded with the 1.2m telescope and McKellar coude
spectrograph at the Dominion Astrophysical Observatory (DAO). The
detector was the 2048x4088pixel SITe-4CCD. The spectrograph was
configured with the IS32R image slicer, the 32inch camera, and the
1200H grating. The central wavelength was set near 6600Å. This
configuration produces a dispersion of 0.15Å/pixel, with a
resolution ∼17000.
Objects:
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RA (2000) DE Designation(s)
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20 47 59.58 +39 17 15.7 V367 Cygni = Gaia DR3 2064979667011780992
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
fig4.dat 26 34770 Mean phase-binned spectra
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See also:
II/179 : Southern Spectrophotometric Standards. I + II (Hamuy+ 1992,94)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/368/932 : BVRI photometry of V367 Cyg (Zola+, 2001)
J/AJ/126/2971 : UBVRI photometry of 131 Herbig Ae/Be (Vieira+, 2003)
J/ApJ/629/1055 : Evolution of close binary systems (Yakut+, 2005)
J/other/BASI/39.517 : Spectroscopy of classical Be stars (Mathew+, 2011)
J/other/Sci/337.444 : RV curves of Galactic massive O stars (Sana+, 2012)
J/MNRAS/491/5489 : Semi-detached double-lined eclipsing bin (Malkov, 2020)
Byte-by-byte Description of file: fig4.dat
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Bytes Format Units Label Explanations
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1- 3 F3.1 --- Phase [0/0.9] Phase bin
5- 16 E12.6 0.1nm Wave [6334/6850] Wavelength; Angstroms
18- 26 E9.3 --- NFlux [0.27/7.32] Normalized flux
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History:
From electronic version of the journal
(End) Prerpared by [AAS], Coralie Fix [CDS], 23-Nov-2022