Abstract:Abstract. We revised the current status of the apsidal-motion test to stellar structure and evolution. The observational sample was increased by about 50% in comparison to previous studies. Classical and relativistic systems were analyzed simultaneously and only systems with accurate absolute dimensions were considered. New interior models incorporating recent opacity tables, stellar rotation, mass loss, and moderate core overshooting were used as theoretical tools to compare the predicted with the observed sh… Show more
“…Before comparing the theoretical and observed k 2 , we carried out a careful comparison of the theoretical and observed absolute dimensions of each system. The comparison with the absolute dimensions of some systems can be found in Claret & Willems (2002) and in Claret (1997). The absolute dimensions of the remaining systems were compared with theoretical values and we found good agreement between values for a given isochrone, as required.…”
Context. The study of apsidal motion in detached eclipsing binary systems is known to be an important source of information about stellar internal structure as well as the possibility of verifying of General Relativity outside the Solar System. Aims. As part of the long-term Ondřejov and Ostrava observational projects, we aim to measure precise times of minima for eccentric eclipsing binaries, needed for the accurate determination of apsidal motion, providing a suitable test of the effects of General Relativity. Methods. About seventy new times of minimum light recorded with photoelectric or CCD photometers were obtained for ten eccentric-orbit eclipsing binaries with significant relativistic apsidal motion. Their O-C diagrams were analysed using all reliable timings found in the literature, and new or improved elements of apsidal motion were obtained. Results. We confirm very long periods of apsidal motion for all systems. For BF Dra and V1094 Tau, we present the first apsidalmotion solution. The relativistic effects are dominant, representing up to 100% of the total observable apsidal-motion rate in several systems. The theoretical and observed values of the internal structure constant k 2 were compared for systems with lower relativistic contribution. Using the light-time effect solution, we predict a faint third component for V1094 Tau orbiting with a short period of about 8 years.
“…Before comparing the theoretical and observed k 2 , we carried out a careful comparison of the theoretical and observed absolute dimensions of each system. The comparison with the absolute dimensions of some systems can be found in Claret & Willems (2002) and in Claret (1997). The absolute dimensions of the remaining systems were compared with theoretical values and we found good agreement between values for a given isochrone, as required.…”
Context. The study of apsidal motion in detached eclipsing binary systems is known to be an important source of information about stellar internal structure as well as the possibility of verifying of General Relativity outside the Solar System. Aims. As part of the long-term Ondřejov and Ostrava observational projects, we aim to measure precise times of minima for eccentric eclipsing binaries, needed for the accurate determination of apsidal motion, providing a suitable test of the effects of General Relativity. Methods. About seventy new times of minimum light recorded with photoelectric or CCD photometers were obtained for ten eccentric-orbit eclipsing binaries with significant relativistic apsidal motion. Their O-C diagrams were analysed using all reliable timings found in the literature, and new or improved elements of apsidal motion were obtained. Results. We confirm very long periods of apsidal motion for all systems. For BF Dra and V1094 Tau, we present the first apsidalmotion solution. The relativistic effects are dominant, representing up to 100% of the total observable apsidal-motion rate in several systems. The theoretical and observed values of the internal structure constant k 2 were compared for systems with lower relativistic contribution. Using the light-time effect solution, we predict a faint third component for V1094 Tau orbiting with a short period of about 8 years.
“…Theoretical values of log k 2 have been computed for the C-04 models in the framework of static tides; for dynamical tides, the effects of the compressibility of the stellar fluid (and resonances, if present) should be also considered (Claret & Willems 2002). For both V760 Sco and U Oph, the observed and theoretical values are in good agreement.…”
Context. Precise stellar masses and radii provide unique information on stellar evolution. In a Galactic context, they may also provide information on the evolution of the Solar neighbourhood. Aims. We aim to determine absolute dimensions for the mid B-type eclipsing binary U Ophiuchi and compare the inferred ages and chemical compositions to those of other binary stars with masses near 5 M . Methods. We determine masses, radii, log g, log T eff , and luminosities for the stars in U Oph from new radial velocities and uvby light curves. By improving the Wilson-Devinney code, we also derive precise apsidal-motion and light-time orbits of this triple system, using 353 times of minimum over 120 years. Finally, we compare the data for U Oph and three similar systems with the predictions of stellar models. Results. The stars in U Oph have masses of 5.27 ± 0.09 M and 4.74 ± 0.07 M , radii of 3.48 ± 0.02 R and 3.11 ± 0.03 R ; we argue that systematic errors are negligible. The apsidal motion period is exceptionally short, U ∼ 21 yr, while the light-time orbit has P 3 ∼ 38.4 yr. The precise log g values for DI Her, U Oph, V760 Sco, and MU Cas, all within 10% of 5 M , place them successively from the ZAMS to the TAMS, at ages of 5−100 × 10 6 yr. Current stellar evolution models fit both stars in each system very well if the (otherwise unconstrained) metal abundance Z is adjusted in each case. Conclusions. More accurate data and/or binary systems with larger mass ratios are needed to actually test stellar models near 5 M . The different Z values found for these young, nearby systems suggest that disk stars form with a range of metal abundances even today, but more data are needed to confirm this result.
“…7.1, V1130 Tau points towards a lower He abundance and/or enrichment ratio than the four different Y, Z prescriptions adopted by the model grids studied. We refer to Casagrande et al (2007) for at recent determination of ΔY/ΔZ based on K dwarfs (2.1 ± 0.9), to Blaser (2006) for a HII based study (1.41 ± 0.62) with references to a variety of methods and results, and to and Claret & Willems (2002) for determinations based on samples of eclipsing binaries (2.2 ± 0.8 and 1.9 ± 0.6, respectively). We believe binaries can give an even better constraint, provided detailed heavy element abundance determinations become available for a sufficiently large sample 10 .…”
Context. 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 1-2 M evolutionary models. Aims. We aim to determine absolute dimensions and abundances for the detached eclipsing binary V1130 Tau, and to perform a detailed comparison with results from recent stellar evolutionary models. Methods. uvby light curves and uvbyβ standard photometry have been obtained with the Strömgren 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. Results. V1130 Tau is a bright (m V = 6.56), nearby (71 ± 2 pc) detached system with a circular orbit (P = 0. d 80). 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 −1 , are in fair agreement with synchronization. The larger 1.39 M secondary component has evolved to the middle of the main-sequence band and is slightly cooler than the 1.31 M 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 2.1 Gyr. All such models are, however, systematically about 200 K 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 V1130 Tau, but on the other hand, we find excellent agreement for 2.5-2.8 Gyr Granada models with a slightly lower Y of 0.23-0.24. Conclusions. V1130 Tau is a valuable addition to the very few well-studied 1-2 M 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.
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