2008A&A...487.1095C


Query : 2008A&A...487.1095C

2008A&A...487.1095C - Astronomy and Astrophysics, volume 487, 1095-1117 (2008/9-1)

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., NORDSTROEM B., STEFANIK R.P., LATHAM D.W. and SOUTHWORTH J.

Abstract (from CDS):

Accurate mass, radius, and abundance determinations from binaries provide important information on stellar evolution, fundamental to central fields in modern astrophysics and cosmology. 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. uvby light curves and uvbyβ standard photometry were obtained with the Stroemgren Automatic Telescope at ESO, La Silla, radial velocity observations at CfA facilities, and supplementary high-resolution spectra with ESO's FEROS spectrograph. State-of-the-art methods were applied for the analyses: the EBOP and Wilson-Devinney binary models, two-dimensional cross-correlation and disentangling, and the VWA abundance analysis tool. 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. 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.

Abstract Copyright:

Journal keyword(s): stars: evolution - stars: fundamental parameters - stars: binaries: close - stars: binaries: eclipsing - techniques: photometric - techniques: spectroscopic

VizieR on-line data: <Available at CDS (J/A+A/487/1095): tablea1.dat tablea2.dat tablea3.dat>

Simbad objects: 12

goto Full paper

goto View the references in ADS

Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* V505 Per EB* 02 21 12.9632050320 +54 30 36.281725236   7.30 6.88     F5 76 0
2 V* CD Tau EB* 05 17 31.1530161432 +20 07 54.627762000 7.27 7.25 6.76     A5:IapHIwk: 159 0
3 V* EW Ori EB* 05 20 09.1431629664 +02 02 40.004288664   10.47 9.78     F8 95 0
4 V* UX Men EB* 05 30 03.1855215048 -76 14 55.350331296   8.80 8.24   7.608 F8V 116 0
5 V* VZ Hya EB* 08 31 41.4131992848 -06 19 07.563903420   9.48 9.06     F3/5V 109 0
6 V* HS Hya EB* 10 24 36.7678198944 -19 05 32.956244232   8.53 8.12     F5V 112 0
7 V* DM Vir EB* 14 07 52.4283264888 -11 09 07.472310912   9.25 8.79     F5V 97 0
8 V* AD Boo EB* 14 35 12.7797940752 +24 38 21.323757120   9.95 9.44     G0 66 0
9 V* WZ Oph EB* 17 06 39.0447030672 +07 46 57.800710560   9.66 9.12     F8 120 0
10 V* V1143 Cyg EB* 19 38 41.1829269072 +54 58 25.647010572       5.6   F6Va 214 0
11 V* BW Aqr EB* 22 23 15.9305850720 -15 19 56.201783268   10.8 10.3     F7 100 0
12 V* IT Cas EB* 23 42 01.3774276248 +51 44 36.818206584   11.57 11.23     F6 69 0

To bookmark this query, right click on this link: simbad:objects in 2008A&A...487.1095C and select 'bookmark this link' or equivalent in the popup menu


2022.10.02-01:56:42

© Université de Strasbourg/CNRS

    • Contact