Absolute Dimensions of the A-Type Eclipsing Binary V364 Lacertae

Torres, Guillermo; Lacy, Claud H.; Claret, A.; Zakirov, M. M.; Arzumanyants, G. C.; Bayramov, N.; Hojaev, A. S.; Stefanik, R. P.; Latham, David W.; Sabby, Jeffrey A.

doi:10.1086/301050

Cited by 22 publications

(12 citation statements)

References 23 publications

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“…Thus, these systems will appear to have anomalously low q values, further adding to the uncertainty in the mass-ratio distribution. (Torres et al 1999) Notes. See text for details.…”

Section: Mass-ratio Distributionmentioning

confidence: 99%

Eclipsing Am binary systems in the SuperWASP survey

Smalley

Southworth

Pintado

et al. 2014

A&A

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The results of a search for eclipsing Am star binaries using photometry from the SuperWASP survey are presented. The light curves of 1742 Am stars fainter than V = 8.0 were analysed for the presence of eclipses. A total of 70 stars were found to exhibit eclipses, with 66 having sufficient observations to enable orbital periods to be determined and 28 of which are newly identified eclipsing systems. Also presented are spectroscopic orbits for 5 of the systems. The number of systems and the period distribution is found to be consistent with that identified in previous radial velocity surveys of "classical" Am stars.

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“…Thus, these systems will appear to have anomalously low q values, further adding to the uncertainty in the mass-ratio distribution. (Torres et al 1999) Notes. See text for details.…”

Section: Mass-ratio Distributionmentioning

confidence: 99%

Eclipsing Am binary systems in the SuperWASP survey

Smalley

Southworth

Pintado

et al. 2014

A&A

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“… References: (1) Brancewicz & Dworak (1980); (2) Kreiner (2004); (3) Popper (1981); (4) Andersen (1991); (5) Lacy (1997a); (6) Balona (1994); (7) Popper (1987); (8) Cester et al (1978b); (9) Liu (1993); (10) Malkov (1993); (11) Deǧirmenci et al (2003); (12) Popper (1980); (13) Popper (1983); (14) Hall & Hubbard (1971); (15) Giuricin & Mardirossian (1981a); (16) Harmanec (1988); (17) Andersen & Vaz (1984); (18) Torres et al (1999); (19) Petrova & Orlov (1999); (20) Andersen, Nordström & Clausen (1990); (21) Munari et al (2001); (22) Deǧirmenci (1997); (23) Lacy (1997b); (24) North, Studer & Kunzli (1997); (25) Mardirossian & Giuricin (1981). …”

Section: Descriptionmentioning

confidence: 99%

A catalogue of close binaries located in the δ Scuti region of the Cepheid instability strip

Soydugan

Demirçan

et al. 2006

Monthly Notices of the Royal Astronomical Society

105

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A catalogue of close eclipsing binary systems (detached and semidetached) with at least one of the components located in the δ Scuti region of the Cepheid instability strip is presented. The positions of the stars in the instability strip are determined by their accurate temperatures and luminosities. Observationally detected binaries (20 semidetached, four detached and one unclassified) with oscillating components were included in the catalogue as a separate table. The primaries of the oscillating Algols tend to be located near the blue edge of the instability strip. Using reliable luminosities and temperatures determined by recent photometric and spectroscopic studies, we have found that at least one or two components of 71 detached and 90 semidetached systems are located in the δ Scuti region of the Cepheid instability strip. In addition, 36 detached or semidetached systems discovered by the Hipparcos satellite were also given as a separate list. One of their components is seen in the δ Scuti region, according to their spectral type or B−V colours. They are potential candidate binaries with the δ Scuti‐type pulsating components which need further photometric and spectroscopic studies in better precision. This catalogue covers information and literature references for 25 known and 197 candidate binaries with pulsating components.

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“…1 References to Burns et al (1996), 2) Andersen et al (1987), 3) Andersen et al (1984), 4) Imbert (1987), 5) Clausen (1991), 6) , 7) Claret et al (1995), 8) , 9) Andersen & Giménez (1985), 10) Giménez & Quintana (1992), 11) , 12) Simon et al (1994), 13) , 14) , 15) Giménez et al (1986), 16) Clausen et al (1986), 17) Holmgren et al (1995), 18) Wolf (1995), 19) Barembaum & Etzel (1995), 20) Clausen (1996), 21) Claret & Giménez (1993), 22) Caton & Burns (1993), 23) , 24) Torres et al (1999), 25) , 26) Andersen (1991), 27) Lacy & Frueh (1985), 28) Andersen et al (1993), 29) Clausen & Giménez (1991), 30) , 31) , 32) Wolf (2000), 33) , 34) ,Acknowledgements. The Spanish DGESIC (project PB98-0499) is acknowledged by the support received.…”

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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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Absolute Dimensions of the A-Type Eclipsing Binary V364 Lacertae

Cited by 22 publications

References 23 publications

Eclipsing Am binary systems in the SuperWASP survey

Eclipsing Am binary systems in the SuperWASP survey

A catalogue of close binaries located in the δ Scuti region of the Cepheid instability strip

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

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