Close binary systems in multiple stars: III. Eclipsing variables with LITE effect

Zakirov, M. M.

doi:10.3103/s0884591310060012

Cited by 6 publications

(8 citation statements)

References 160 publications

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“…The lack of short period companions is consistent with other results on tertiary companions of spectroscopic binaries (Tokovinin et al 2006) and on those previously found through LITE methods (Zakirov 2010). Tokovinin et al (2006) made an adaptive optics survey of nearby, spectroscopic binaries consisting of solar-type stars.…”

Section: Discussionsupporting

confidence: 89%

“…Such a statement must await a longer time span of observations that shows true periodic variability in the O − C residuals for both eclipses. In the meantime, we caution that long-term secular variations associated with mass exchange, systemic mass loss, tidal dissipation, and magnetic cycles may be present in some systems (Tokovinin et al 2006;Pilecki et al 2007;Zakirov 2010). However, there are some situations where the evidence does indeed point towards the third body explanation.…”

Section: Discussionmentioning

confidence: 85%

“…The triple star system IU Aur may represent an example where such dynamical perturbations influence the eclipse timings ( Özdemir et al 2003). Eclipse timing observations have led to the identification of many candidate binaries with tertiary companions (Liao & Qian 2010;Zakirov 2010) and even the detection of planets around a binary (Lee et al 2009). However, caution is required in the interpretation of trends in the eclipse times since other long-term, secular processes can also affect the angular momentum of the orbit (Zavala et al 2002;Hoffman et al 2006;Pilecki et al 2007).…”

Section: Introductionmentioning

confidence: 99%

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A SEARCH FOR HIERARCHICAL TRIPLES USINGKEPLERECLIPSE TIMING

Gies¹,

Williams²,

Matson³

et al. 2012

The Astronomical Journal

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We produce and analyze eclipse time variation (ETV) curves for some 2600 targeted main-field Kepler binaries. We find good to excellent evidence for a third body in 222 systems via either the light-travel-time (LTTE) or dynamical effect delays. Approximately half of these systems have been discussed in previous work, while the rest are newly reported here. Via detailed analysis of the ETV curves using high-level analytic approximations, we are able to extract system masses and information about the three-dimensional characteristics of the triple for 62 systems which exhibit both LTTE and dynamical delays. For the remaining 160 systems whose ETV curves are dominated by LTTE delays we are able to extract the outer orbital period, eccentricity , and longitude of periastron as well as the mass function of the triple. In general, our solutions improve upon those published earlier. New techniques of preprocessing the flux time series are applied to eliminate false positive triples and to enhance the ETV curves. The set of triples with outer orbital periods shorter than ∼2000 days is now sufficiently numerous for meaningful statistical analysis. We find that (i) as predicted, there is a peak near i m 40 • in the distribution of the triple vs. inner binary mutual inclination angles that provides strong confirmation of the operation of Kozai-Lidov cycles with tidal friction; (ii) the median eccentricity of the third-body orbits is e 2 = 0.35; (iii) there is a deficit of triple systems with binary periods 1 day and outer periods between ∼50 and 200 days which might help guide the refinement of theories of the formation and evolution of close binaries; and (iv) the substantial fraction of Kepler binaries which have third-body companions is consistent with a very large fraction of all binaries being part of triples.

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Section: Discussionsupporting

confidence: 89%

Section: Discussionmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

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A SEARCH FOR HIERARCHICAL TRIPLES USINGKEPLERECLIPSE TIMING

Gies¹,

Williams²,

Matson³

et al. 2012

The Astronomical Journal

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show abstract

“…The method of period analysis, despite its classical nature and many decades of usage (about 250 such systems known nowadays, see e.g. Zakirov 2010), still provides us with an efficient method of discovering the hidden components in the eclipsing systems. Its main advantage is the easiness of use because of huge datasets of times of eclipses.…”

Section: Introductionmentioning

confidence: 99%

THE PERIOD ANALYSIS OF V418 AQL, SU BOO, RV CVn, CR CAS, GV CYG, V432 PER, AND BD+42 2782

Zasche

Wolf

Uhlàř³

et al. 2014

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The minimum timings of eclipsing binaries V418 Aql, SU Boo, RV CVn, CR Cas, GV Cyg, V432 Per, and BD+42 2782 were collected and analyzed. Their long-term behavior was studied via period analysis, revealing a periodic term in eclipse times. We derived 576 new times of minimum. Hence, to describe the periodic variation, a thirdbody hypothesis was proposed and the resulting orbital periods are as follows: 70, 7.4, 53, 37, 27, 53, and 18 yr, respectively. For the system V432 Per an additional 9.5 yr variation was also found. The predicted minimum masses of these distant bodies were calculated and their detectability discussed. The light curves of SU Boo and RV CVn were analyzed using the PHOEBE program, resulting in physical parameters of the components. New variable stars in the field of V418 Aql were discovered.

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“…Theoretical studies suggest that a significant number of close binaries have a distant tertiary companion which plays an important role in the evolution of the inner binary through the exchange of angular momentum (Eggleton & Kisseleva-Eggleton 2006;Fabrycky & Tremaine 2007;Naoz & Fabrycky 2014). Observational evidence of such systems has been found by Pribulla & Rucinski (2006), Tokovinin et al (2006), Raghavan et al (2010), and Zakirov (2010). Kepler has managed to increase the discovery of close binaries with tertiary companions (Carter et al 2011;Lee et al 2013;Rappaport et al 2013;Borkovits et al 2013Borkovits et al , 2015Lee et al 2015) and provide insight into the stability, dynamics, and evolution of such systems.…”

Section: Introductionmentioning

confidence: 99%

Fundamental Parameters of Kepler Eclipsing Binaries. I. Kic 5738698

Matson

Gies

Guo

et al. 2016

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Eclipsing binaries serve as a valuable source of stellar masses and radii that inform stellar evolutionary models and provide insight into additional astrophysical processes. The exquisite light curves generated by space-based missions such as Kepler offer the most stringent tests to date. We use the Kepler light curve of the 4.8 day eclipsing binary KIC 5739896 with ground based optical spectra to derive fundamental parameters for the system. We reconstruct the component spectra to determine the individual atmospheric parameters, and model the Kepler photometry with the binary synthesis code ELC to obtain accurate masses and radii. The two components of KIC 5738698 are F-type stars with M 1 = 1.39 ± 0.04M , M 2 = 1.34 ± 0.06M , and R 1 = 1.84 ± 0.03R , R 2 = 1.72 ± 0.03R . We also report a small eccentricity (e 0.0017) and unusual albedo values that are required to match the detailed shape of the Kepler light curve. Comparison with evolutionary models indicate an approximate age of 2.3 Gyr for the system.

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Close binary systems in multiple stars: III. Eclipsing variables with LITE effect

Cited by 6 publications

References 160 publications

A SEARCH FOR HIERARCHICAL TRIPLES USINGKEPLERECLIPSE TIMING

A SEARCH FOR HIERARCHICAL TRIPLES USINGKEPLERECLIPSE TIMING

THE PERIOD ANALYSIS OF V418 AQL, SU BOO, RV CVn, CR CAS, GV CYG, V432 PER, AND BD+42 2782

Fundamental Parameters of Kepler Eclipsing Binaries. I. Kic 5738698

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