Absolute dimensions and masses of IT cassiopeiae.

Lacy, Claud H.; Torres, Guillermo; Latham, David W.; Zakirov, M. M.; Arzumanyants, G. C.

doi:10.1086/118553

Cited by 19 publications

(13 citation statements)

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“…5 and 6 and is denoted by a star. However, we did not consider this system in our present investigation since there seems to be a discrepancy in its observed apsidal-motion rate (Lacy et al 1997;Kozyreva & Zakharov 2001). …”

Section: Comparison With Observationsmentioning

confidence: 95%

New results on the apsidal-motion test to stellar structure and evolution including the effects of dynamic tides

Claret

Willems²

2002

A&A

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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 shifts of the position of the periastron. The stellar models were computed for the precise observed masses and the adopted chemical compositions are consistent with the corresponding tables of opacities to avoid the inherent problems of interpolation in mass and in (X, Z). The derived chemical composition for each individual system was used to infer the primordial helium content as well as a law of enrichment. The values found are in good agreement with those obtained from various independent sources. For the first time, the effects of dynamic tides are taken into account systematically to determine the contribution of the tidal distortion to the predicted apsidal-motion rate. The deviations between the apsidal-motion rates resulting from the classical formula and those determined by taking into account the effects of dynamic tides are presented as a function of the level of synchronism. For systems close to synchronisation, dynamic tides cause deviations with respect to the classical apsidal-motion formula due to the effects of the compressibility of the stellar fluid. For systems with higher rotational angular velocities, additional deviations due to resonances arise when the forcing frequencies of the dynamic tides come into the range of the free oscillation modes of the component stars. The resulting comparison shows a good agreement between the observed and theoretical apsidal-motion rates. No systematic effects in the sense that models are less mass concentrated than real stars and no correlations with the evolutionary status of the systems were detected.

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Section: Comparison With Observationsmentioning

confidence: 95%

New results on the apsidal-motion test to stellar structure and evolution including the effects of dynamic tides

Claret

Willems²

2002

A&A

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“…See also history summarized in that paper. Accurate masses and radii was determined spectroscopically by Lacy et al (1997), who detected components of similar mass and size (see Table 3). They also excluded the previous reports of δ Scuti variations.…”

Section: It Casmentioning

confidence: 99%

“…Apart from the minima given in Table A.1, we add numerous times of minimum obtained by several observers: Lacy et al (1997, their Table 4, 1998), Agerer & Hübscher (2003), Diethelm (2003), Nakajima (2003) 3 , Hübscher (2005), Hübscher et al (2005), Smith & Caton (2007), and Hübscher & Walter (2007). A total of 95 times of minimum are now available, of which 51 correspond to primary eclipses and 44 to secondary eclipses (Table A.2).…”

Section: It Casmentioning

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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“…The occurrence of a third object in the system of GSC 3822-1056 is not unprecedented, but it has relatively high luminosity compared to the close pair. Note that V909 Cygni (although it is an Algol-star object) also has high fractional luminosity third companion (in that case L 3 /L total ≈ 0.22 in B and V, Lacy et al 1999). Other Algols, as AC Vel (10-15% third light in y, Johanssen et al 1997) and DI Peg (22-25% third light in V, Rucinski 1967) also have large third light.…”

Section: Light Curve Solutionmentioning

confidence: 99%

Photometric study of the over-contact binary star GSC 3822-1056

Csizmadia

Bíró

Borkovits³

2003

A&A

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Abstract.Here we present the first Johnson-Cousins VR C light curves of the over-contact binary star GSC 3822-1056. A period study and the light curve solution are also given. An extremely high rate of period increase (+11.6 s/century) was found. The origin of this period change can be: (i) partly covered light-time effect due to the orbital motion around the mass center of a possible third body; (ii) mass transfer between the components. The light curve was solved using the 1998 Wilson-Devinney Code. We examined the light curve with and without third light. Both solutions yielded a contact configuration with high temperature difference between the components. Despite the high degree of the contact ( f = 0.57), the temperature difference between the components ∆T = T primary − T secondary = 1045 K. The high mass ratio of the system and its other unusual properties suggest that GSC 3822-1056 may be a recently formed contact binary.

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Absolute dimensions and masses of IT cassiopeiae.

Cited by 19 publications

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New results on the apsidal-motion test to stellar structure and evolution including the effects of dynamic tides

New results on the apsidal-motion test to stellar structure and evolution including the effects of dynamic tides

Relativistic apsidal motion in eccentric eclipsing binaries

Photometric study of the over-contact binary star GSC 3822-1056

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