SPECTROSCOPIC METALLICITY DETERMINATIONS FOR W UMa-TYPE BINARY STARS

This study is the first attempt to determine the metallicities of W UMa-type binary stars using spectroscopy. We analyzed about 4500 spectra collected at the David Dunlap Observatory. To circumvent problems caused by the extreme spectral line broadening and blending and by the relatively low quality...

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Veröffentlicht in:The Astronomical journal Jg. 146; H. 3; S. 70 - 20
Hauptverfasser: Rucinski, Slavek M., Pribulla, Theodor, Budaj, Ján
Format: Journal Article
Sprache:Englisch
Veröffentlicht: United States 01.09.2013
Schlagworte:
Astronomical instruments
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BINARY STARS
Blending
COLOR
LINE BROADENING
MASS
Mathematical models
Metallicity
METALS
PHOTOMETRY
PROPER MOTION
RADIAL VELOCITY
SPECTRA
Spectral lines
SPECTROSCOPY
STELLAR ATMOSPHERES
Strength
ISSN:0004-6256, 1538-3881, 1538-3881
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Abstract This study is the first attempt to determine the metallicities of W UMa-type binary stars using spectroscopy. We analyzed about 4500 spectra collected at the David Dunlap Observatory. To circumvent problems caused by the extreme spectral line broadening and blending and by the relatively low quality of the data, all spectra were subject to the same broadening function (BF) processing to determine the combined line strength in the spectral window centered on the Mg I triplet between 5080 A and 5285 A. All individual integrated BFs were subsequently orbital-phase averaged to derive a single line-strength indicator for each star. The best defined results were obtained for an F-type sub-sample (0.32 < (B - V) sub(0) < 0.62) of 52 binaries for which integrated BF strengths could be interpolated in the model atmosphere predictions.
AbstractList This study is the first attempt to determine the metallicities of W UMa-type binary stars using spectroscopy. We analyzed about 4500 spectra collected at the David Dunlap Observatory. To circumvent problems caused by the extreme spectral line broadening and blending and by the relatively low quality of the data, all spectra were subject to the same broadening function (BF) processing to determine the combined line strength in the spectral window centered on the Mg I triplet between 5080 A and 5285 A. All individual integrated BFs were subsequently orbital-phase averaged to derive a single line-strength indicator for each star. The best defined results were obtained for an F-type sub-sample (0.32 < (B - V) sub(0) < 0.62) of 52 binaries for which integrated BF strengths could be interpolated in the model atmosphere predictions.
This study is the first attempt to determine the metallicities of W UMa-type binary stars using spectroscopy. We analyzed about 4500 spectra collected at the David Dunlap Observatory. To circumvent problems caused by the extreme spectral line broadening and blending and by the relatively low quality of the data, all spectra were subject to the same broadening function (BF) processing to determine the combined line strength in the spectral window centered on the Mg I triplet between 5080 A and 5285 A. All individual integrated BFs were subsequently orbital-phase averaged to derive a single line-strength indicator for each star. The star sample was limited to 90 W UMa-type (EW) binaries with the strict phase-constancy of colors and without spectral contamination by spectroscopic companions. The best defined results were obtained for an F-type sub-sample (0.32 < (B - V){sub 0} < 0.62) of 52 binaries for which integrated BF strengths could be interpolated in the model atmosphere predictions. The logarithmic relative metallicities, [M/H], for the F-type sub-sample indicate metal abundances roughly similar to the solar metallicity, but with a large scatter which is partly due to combined random and systematic errors. Because of the occurrence of a systematic color trend resulting from inherent limitations in our approach, we were forced to set the absolute scale of metallicities to correspond to that derived from the m{sub 1} index of the Stroemgren uvby photometry for 24 binaries of the F-type sub-sample. The trend-adjusted metallicities [M/H]{sub 1} are distributed within -0.65 < [M/H]{sub 1} < +0.50, with the spread reflecting genuine metallicity differences between stars. One half of the F-sub-sample binaries have [M/H]{sub 1} within -0.37 < [M/H]{sub 1} < +0.10, a median of -0.04 and a mean of -0.10, with a tail toward low metallicities, and a possible bias against very high metallicities. A parallel study of kinematic data, utilizing the most reliable and recently obtained proper motion and radial velocity data for 78 binaries of the full sample, shows that the F-type sub-sample binaries (44 stars with both velocities and metallicity determinations) have similar kinematic properties to solar-neighborhood, thin-disk dwarfs with space velocity component dispersions: {sigma}U = 33 km s{sup -1}, {sigma}V = 23 km s{sup -1} and {sigma}W = 14 km s{sup -1}. FU Dra with a large spatial velocity, V{sub tot} = 197 km s{sup -1} and [M/H]{sub 1} = -0.6 {+-} 0.2, appears to be the only thick-disk object in the F-type sub-sample. The kinematic data indicate that the F-type EW binaries are typical, thin-disk population stars with ages about 3-5.5 Gyr. The F-type binaries that appear to be older than the rest tend to have systematically smaller mass ratios than most of the EW binaries of the same period.
Author Pribulla, Theodor
Budaj, Ján
Rucinski, Slavek M.
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BackLink https://www.osti.gov/biblio/22136544$$D View this record in Osti.gov
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Snippet This study is the first attempt to determine the metallicities of W UMa-type binary stars using spectroscopy. We analyzed about 4500 spectra collected at the...
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SubjectTerms Astronomical instruments
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BINARY STARS
Blending
COLOR
LINE BROADENING
MASS
Mathematical models
Metallicity
METALS
PHOTOMETRY
PROPER MOTION
RADIAL VELOCITY
SPECTRA
Spectral lines
SPECTROSCOPY
STELLAR ATMOSPHERES
Strength
Title SPECTROSCOPIC METALLICITY DETERMINATIONS FOR W UMa-TYPE BINARY STARS
URI https://www.proquest.com/docview/1680462475
https://www.proquest.com/docview/1685809965
https://www.osti.gov/biblio/22136544
Volume 146
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