Absolute dimensions of eclipsing binaries. XXVI, Setting a new standard : masses, radii, and abundances for the F-type systems AD Bootis, VZ Hydrae, and WZ Ophiuchi
Clausen, J. V., Torres, G., Bruntt, H., Andersen, J. (Johannes), Nordström, Birgitta, Stefanik, R. P., Latham, David W. and Southworth, J. (John). (2008) Absolute dimensions of eclipsing binaries. XXVI, Setting a new standard : masses, radii, and abundances for the F-type systems AD Bootis, VZ Hydrae, and WZ Ophiuchi. Astronomy & Astrophysics, Vol.487 (No.3). pp. 1095-1117. ISSN 0004-6361
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Official URL: http://dx.doi.org/10.1051/0004-6361:200809671
Context. Accurate mass, radius, and abundance determinations from binaries provide important information on stellar evolution, fundamental to central fields in modern astrophysics and cosmology.
Aims. We aim to determine absolute dimensions and abundances for the three F-type main-sequence detached eclipsing binaries ADBoo, VZHya, and WZOph and to perform a detailed comparison with results from recent stellar evolutionary models.
Methods. uvby light curves and uvbyβ standard photometry were obtained with the Strömgren Automatic Telescope at ESO, La Silla, radial velocity observations at CfA facilities, and supplementary high-resolution spectra with ESO’s FEROS spectrograph. State-ofthe-art methods were applied for the analyses: the EBOP andWilson-Devinney binary models, two-dimensional cross-correlation and
disentangling, and the VWA abundance analysis tool.
Results. Masses and radii that are precise to 0.5–0.7% and 0.4–0.9%, respectively, have been established for the components, which span the ranges of 1.1 to 1.4 M and 1.1 to 1.6 R. The [Fe/H] abundances are from –0.27 to +0.10, with uncertainties between 0.07 and 0.15 dex. We find indications of a slight α-element overabundance of [α/Fe] ∼ +0.1 for WZOph. The secondary component of ADBoo and both components of WZOph appear to be slightly active. Yale-Yonsai and Victoria-Regina evolutionary models fit the
components of ADBoo and VZHya almost equally well, assuming coeval formation, at ages of about 1.75/1.50 Gyr (ADBoo) and
1.25/1.00 Gyr (VZHya). BaSTI models, however, predict somewhat different ages for the primary and secondary components. For WZOph, the models from all three grids are significantly hotter than observed. A low He content, decreased envelope convection coupled with surface activity, and/or higher interstellar absorption would remove the discrepancy, but its cause has not been definitively identified.
Conclusions. We have demonstrated the power of testing and comparing recent stellar evolutionary models using eclipsing binaries, provided their abundances are known. The strongest limitations and challenges are set by Teff and interstellar absorption determinations, and by their effects on and correlation with abundance results.
|Item Type:||Journal Article|
|Subjects:||Q Science > QB Astronomy|
|Divisions:||Faculty of Science > Physics|
|Library of Congress Subject Headings (LCSH):||Eclipsing binaries, Stars -- Evolution, Double stars -- Masses, Cosmic abundances|
|Journal or Publication Title:||Astronomy & Astrophysics|
|Publisher:||E D P Sciences|
|Official Date:||September 2008|
|Page Range:||pp. 1095-1117|
|Access rights to Published version:||Open Access|
|Funder:||Danmarks Grundforskningsfond [Danish National Research Foundation], National Science Foundation (U.S.) (NSF), Carlsbergfondet (Copenhagen, Denmark) [Carlsberg foundation], United States. National Aeronautics and Space Administration (NASA)|
|Grant number:||AST-0406183 (NSF), AST-0708229 (NSF)|
Alonso, A., Arribas, S., & Martínez-Roger, C. 1996, A&A, 313, 873
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