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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Bibliographic Details
Published in:The Astronomical journal Vol. 146; no. 3; pp. 70 - 20
Main Authors: Rucinski, Slavek M., Pribulla, Theodor, Budaj, Ján
Format: Journal Article
Language:English
Published: United States 01.09.2013
Subjects:
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
Online Access:Get full text
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Summary: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.
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content type line 23
ISSN:0004-6256
1538-3881
1538-3881
DOI:10.1088/0004-6256/146/3/70