New grids of stellar models including tidal-evolution constants up to carbon burning

Claret, A.

doi:10.1051/0004-6361:20040470

Cited by 294 publications

(407 citation statements)

References 21 publications

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“…The apsidal-motion test will only be reliable if the adopted stellar models are capable of reproducing the absolute dimensions. The grids of stellar models used here are based on the code described in detail in Claret (2004). The convective core overshooting is introduced by means of an excess distance beyond the classical convective border (see also Claret 2007).…”

Section: Discussionmentioning

confidence: 99%

Relativistic apsidal motion in eccentric eclipsing binaries

Wolf¹,

Claret²,

Kotková

et al. 2010

A&A

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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.

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Section: Discussionmentioning

confidence: 99%

Relativistic apsidal motion in eccentric eclipsing binaries

Wolf¹,

Claret²,

Kotková

et al. 2010

A&A

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“…We have also considered a second set of models, from the series by Claret (2004). The physics in these calculations is similar, though not exactly the same as the previous ones.…”

Section: Comparison With Stellar Evolution Theorymentioning

confidence: 91%

Absolute Properties of the Spotted Eclipsing Binary Star Cv Boötis

Torres

Vaz

Lacy

2008

The Astronomical Journal

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We present new V-band differential brightness measurements as well as new radial-velocity measurements of the detached, circular, 0.84 day period, double-lined eclipsing binary system, CV Boo. These data, along with other observations from the literature, are combined to derive improved absolute dimensions of the stars for the purpose of testing various aspects of theoretical modeling. Despite complications from intrinsic variability that we detect in the system, and despite the rapid rotation of the components, we are able to determine the absolute masses and radii to better than 1.3% and 2%, respectively. We obtain M A = 1.032 ± 0.013 M and R A = 1.262 ± 0.023 R for the hotter, larger, and more-massive primary (star A), and M B = 0.968 ± 0.012 M and R B = 1.173 ± 0.023 R for the secondary. The estimated effective temperatures are 5760 ± 150 K and 5670 ± 150 K, respectively. The intrinsic variability with a period ∼1% shorter than the orbital period is interpreted as being due to modulation by spots on one or both components. This implies that the spotted star(s) must be rotating faster than the synchronous rate, which disagrees with predictions from current tidal evolution models according to which both stars should be synchronized. We also find that the radius of the secondary is larger than expected from stellar evolution calculations by ∼10%, a discrepancy also seen in other (mostly lower-mass and active) eclipsing binaries. We estimate the age of the system to be approximately 9 Gyr. Both components are near the end of their main-sequence phase, and the primary may have started the shell hydrogen-burning stage.

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“…(28) and (29)). The only available modern calculations that provide E 2 values are the models computed by Claret (2004Claret ( , 2005Claret ( , 2006Claret ( , 2007 which include core overshooting. Comparison between the 5 M , Z = 0.02 model of Claret (2004) and our 5 M with similar physics, reveals noticeable discrepancies.…”

Section: Tidal Timescale In Main Sequence Stars With Radiative Envelopesmentioning

confidence: 99%

BINSTAR: a new binary stellar evolution code

Siess

Izzard

Davis

et al. 2013

A&A

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We provide a detailed description of a new stellar evolution code, BINSTAR, which has been developed to study interacting binaries. Based on the stellar evolution code STAREVOL, it is specifically designed to study low-and intermediate-mass binaries. We describe the state-of-the-art input physics, which includes treatments of tidal interactions, mass transfer and angular momentum exchange within the system. A generalised Henyey method is used to solve simultaneously the stellar structure equations of each component as well as the separation and eccentricity of the orbit. Test simulations for cases A and B mass transfer are presented and compared with available models. The results of the evolution of Algol systems are in remarkable agreement with the calculations of the Vrije Universiteit Brussel (VUB) group, thus validating our code. We also computed a large grid of models for various masses (2 ≤ M/M ≤ 20) and seven metallicities (Z = 0.0001, 0.001, 0.004, 0.008, 0.01, 0.02, 0.03) to provide a useful analytical parameterisation of the tidal torque constant E 2 , which allows the determination of the circularisation and synchronisation timescales for stars with a radiative envelope and convective core. The evolution of E 2 during the main sequence shows noticeable differences compared to available models. In particular, our new calculations indicate that the circularisation timescale is constant during core hydrogen burning. We also show that E 2 weakly depends on core overshooting but is substantially increased when the metallicity becomes lower.

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New grids of stellar models including tidal-evolution constants up to carbon burning

Cited by 294 publications

References 21 publications

Relativistic apsidal motion in eccentric eclipsing binaries

Relativistic apsidal motion in eccentric eclipsing binaries

Absolute Properties of the Spotted Eclipsing Binary Star Cv Boötis

BINSTAR: a new binary stellar evolution code

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