2010A&A...510A..91C


Query : 2010A&A...510A..91C

2010A&A...510A..91C - Astronomy and Astrophysics, volume 510, A91-91 (2010/2-1)

Absolute dimensions of eclipsing binaries. XXVII. V1130 Tauri: a metal-weak F-type system, perhaps with preference for y = 0.23-0.24.

CLAUSEN J.V., OLSEN E.H., HELT B.E. and CLARET A.

Abstract (from CDS):

Double-lined, detached eclipsing binaries are our main source for accurate stellar masses and radii. This paper is the first in a series with focus on the upper half of the main-sequence band and tests of 1-2M evolutionary models. We aim to determine absolute dimensions and abundances for the detached eclipsing binary 4, and to perform a detailed comparison with results from recent stellar evolutionary models. uvby light curves and uvbyβ standard photometry have been obtained with the Stroemgren Automatic Telescope, and high-resolution spectra have been acquired at the FEROS spectrograph; both are ESO, La Silla facilities. We have applied the Wilson-Devinney model for the photometric analysis, spectroscopic elements are based on radial velocities measured via broadening functions, and [Fe/H] abundances have been determined from synthetic spectra and uvby calibrations. 4 is a bright (mV=6.56), nearby (71±2pc) detached system with a circular orbit (P=0.80d). The components are deformed with filling factors above 0.9. Their masses and radii have been established to 0.6-0.7%. We derive a [Fe/H] abundance of -0.25±0.10. The measured rotational velocities, 92.4±1.1 (primary) and 104.7±2.7 (secondary) km/s, are in fair agreement with synchronization. The larger 1.39M secondary component has evolved to the middle of the main-sequence band and is slightly cooler than the 1.31M primary. Yonsai-Yale, BaSTI, and Granada evolutionary models for the observed metal abundance and a ``normal'' He content of Y=0.25-0.26, marginally reproduce the components at ages between 1.8 and 2.1Gyr. All such models are, however, systematically about 200K hotter than observed and predict ages for the more massive component, which are systematically higher than for the less massive component. These trends can not be removed by adjusting the amount of core overshoot or envelope convection level, or by including rotation in the model calculations. They may be due to proximity effects in 4, but on the other hand, we find excellent agreement for 2.5-2.8Gyr Granada models with a slightly lower Y of 0.23-0.24. 4 is a valuable addition to the very few well-studied 1-2M binaries with component(s) in the upper half of the main-sequence band, or beyond. The stars are not evolved enough to provide new information on the dependence of core overshoot on mass (and abundance), but might - together with a larger sample of well-detached systems - be useful for further tuning of the helium enrichment law. Analyses of such systems are in progress.

Abstract Copyright:

Journal keyword(s): stars: evolution - stars: fundamental parameters - stars: individual: V1130 Tau - binaries: eclipsing - techniques: photometric - techniques: radial velocities

VizieR on-line data: <Available at CDS (J/A+A/510/A91): table11.dat>

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* AI Phe SB* 01 09 34.1924055096 -46 15 56.071719360   9.26 8.60     G3V 141 0
2 NGC 752 OpC 01 56 54 +37 47.6           ~ 608 0
3 V* DS And SB* 01 57 46.0564787701 +38 04 28.431446959   10.89 10.52     F5.7 75 0
4 V* V505 Per EB* 02 21 12.9632050320 +54 30 36.281725236   7.30 6.88     F5 76 0
5 V* V570 Per SB* 03 09 34.9441274976 +48 37 28.696544364   8.55 8.09     F5 48 0
6 HD 23503 PM* 03 45 44.5334104824 +00 37 02.228616984   8.69 8.24     F2/3V 23 0
7 V* V1130 Tau SB* 03 50 41.9411242656 +01 33 50.219292672   7.03 6.66     F2V 59 0
8 HD 24552 PM* 03 54 22.6333137168 +01 15 41.830993368   8.58 7.97     G1V 47 0
9 HD 25059 PM* 03 58 56.1792753408 +00 45 04.120613172       8.8   G3V 31 1
10 V* GX Gem EB* 06 46 09.1272024000 +34 24 52.792971336   11.99 11.71     G5 59 0
11 HD 76196 SB* 08 53 50.0707819440 -25 05 03.327352152   9.50 8.96     F5IV/V 5 0
12 V* AL Leo EB* 09 58 12.9052965096 +18 17 28.141323072   10.26 9.89     F5 38 0
13 V* DW Car EB* 10 43 10.0815693384 -60 02 11.745452652 9.02 9.83 9.85 10.03 9.59 B1III 70 0
14 V* V380 Cyg EB* 19 50 37.3267754400 +40 35 59.135141652 4.86 5.613 5.680     B1.1III+B2.5/3V: 283 0
15 V* BW Aqr SB* 22 23 15.9305850720 -15 19 56.201783268   10.8 10.3     F7 101 0
16 V* BK Peg SB* 23 47 08.4664310208 +26 33 59.970121200   10.46 10.04     F8 74 0

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2023.02.01-21:08:28

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