Updated study of the quintuple system V994 Herculis

Zasche, P.; Uhlàř, R.

doi:10.1051/0004-6361/201628153

Cited by 22 publications

(16 citation statements)

References 14 publications

(32 reference statements)

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“…One way to determine whether two eclipsing binaries producing a blended lightcurve are physically bound is to find anti-correlated eclipse timing variations (ETV) in the two pairs. Similar anti-correlated ETVs have proven the real, bound 2+2 quadruple nature of V994 Her (Lee et al 2008;Zasche & Uhlař 2016) and EPIC 220204960 (Rappaport et al 2017). More recently, Zasche et al (2019) performed a thorough analysis of a larger sample of doubly eclipsing binaries found within the frame of Table 2.…”

Section: Period Studymentioning

confidence: 61%

TIC 278956474: Two Close Binaries in One Young Quadruple System Identified by TESS

Rowden

Borkovits

Jenkins

et al. 2020

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We have identified a quadruple system with two close eclipsing binaries in TESS data. The object is unresolved in Gaia and appears as a single source at parallax 1.08 ±0.01 mas. Both binaries have observable primary and secondary eclipses and were monitored throughout TESS Cycle 1 (sectors 1-13), falling within the TESS Continuous Viewing Zone. In one eclipsing binary (P = 5.488 d), the smaller star is completely occluded by the larger star during the secondary eclipse; in the other (P = 5.674 d) both eclipses are grazing. Using these data, spectroscopy, speckle photometry, SED analysis and evolutionary stellar tracks, we have constrained the masses and radii of the four stars in the two eclipsing binaries. The Li I EW indicates an age of 10-50 Myr and, with an outer period of 858 +7 −5 days, our analysis indicates this is one of the most compact young 2+2 quadruple systems known.

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Section: Period Studymentioning

confidence: 61%

TIC 278956474: Two Close Binaries in One Young Quadruple System Identified by TESS

Rowden

Borkovits

Jenkins

et al. 2020

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“…The most complete information is available for V994 Her. Given the masses and orbital periods from Zasche & Uhlař (2016) the ratio of semimajor axes is = a B /a c = 0.014. Resonant capture requires that the initial eccentricity e B0 5/3 0.001 (eq.…”

Section: Discussionmentioning

confidence: 99%

Resonant capture in quadruple stellar systems

Tremaine

2020

Monthly Notices of the Royal Astronomical Society

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Some quadruple star systems in the hierarchical 2+2 configuration exhibit orbit-orbit resonances between the two compact binaries. We show that the most important resonances occur at period ratios of 1:1, 3:2 and 2:1. We describe the conditions required for capture and show that they can be satisfied at the 3:2 and 2:1 resonances in binaries that migrate significantly in semimajor axis after circularization, probably through magnetic braking or gravitational radiation.Quadruple stellar systems are almost always found in hierarchical configurations, since this is the only simple way to ensure long-term orbital stability. There are two possible architectures: the 3+1 configuration, in which a hierarchical triple system is orbited by an even more distant companion, and the 2+2 configuration, in which two relatively compact binaries orbit their common center of mass. In this paper we explore novel resonant phenomena that can arise in the 2+2 configuration.The best-studied 2+2 systems are those in which both compact binaries are eclipsing. These 'doubly eclipsing' systems are rare: the most recent compilation (Zasche et al. 2019) lists only 146 systems, and a significant fraction of these may be superimposed pairs of unrelated eclipsing binaries.Despite the modest sample size, Zasche et al. (2019) find significant peaks in the distribution of period ratios P B /P A near 1 and 1.5 (see Figure 1). There is no evidence for peaks near other resonances such as P B /P A = 2.Here are more complete descriptions of a few of the near-resonant systems from this sample.• V994 Her (Lee et al. 2008; Zasche & Uhlař 2016) consists of two detached eclipsing binary systems with periods P A = 1.4200 d, P B = 2.0833 d. (Here and throughout the paper, the labels 'A' and 'B' refer to the binaries with the shorter and longer periods, and 'C' refers to the mutual orbit of the centers of mass of binaries A and B. Not all authors follow this convention.) The distance is 320 ± 10 pc based on the Gaia DR2 parallax of 3.05 ± 0.13 mas and an assumed parallax offset of 0.05 mas. System A has spectral types A2V and A4V, while B has spectral types B8V and A0V. The stellar masses range from 1.8M to 3.0M ; the main-sequence lifetime of the most massive star is about 3 × 10 8 yr, suggesting that the age of the system is less than this. Both systems have non-zero eccentricities: e A = 0.125 ± 0.007 and e B = 0.031 ± 0.001. The mutual orbit has period P C = 2.91 ± 0.14 yr and eccentricity e C = 0.76 ± 0.07. The period ratio is close to but not exactly 3:2, with 1 − 2P B /3P A = 0.0220.• OGLE BLG-ECL-145467 (Zasche et al. 2019) has P A = 3.305 d, P B = 4.910 d, P C = 1540 ± 90 d. The distance is 3100 ± 400 pc based on the Gaia DR2 parallax of 0.374 ± 0.048 mas and the same assumed parallax offset. All three orbits have non-zero eccentricity, e A = 0.007 ± 0.001, e B = 0.068 ± 0.003, and e C = 0.395 ± 0.018. Apsidal motion is detected in binary A with 2π/ 125 yr. The stars appear to have spectral types near B9. The period ratio is close to a 3:2 resonance, ...

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“…Then, Zasche & Uhlař [190] pointed out that the ETV curves of the two EBs (P in,A = 2.08 d; P in,B = 1.42 d) show anticorrelated behaviour, robustly implying that they form a relatively close 2 + 2 quadruple system. Finally, with the use of new additional eclipse times, Zasche & Uhlař [191] determined the outer period to be…”

Section: Double (Multiple) Ebsmentioning

confidence: 99%

Eclipsing Binaries in Dynamically Interacting Close, Multiple Systems

Borkovits

2022

Galaxies

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Close, compact, hierarchical, and multiple stellar systems, i.e., multiples having an outer orbital period from months to a few years, comprise a small but continuously growing group of the triple and multiple star zoo. Many of them consist of at least one eclipsing pair of stars and, therefore, exhibit readily observable short-term dynamical interactions among the components. Thus, their dynamical and astrophysical properties can be explored with high precision. In this paper we present an overview of the history of the search for additional components around eclipsing binaries from the first serendipitous discoveries to more systematic recent studies. We describe the different observational detection methods and discuss their connections to the different kinds of astrophysical and dynamical information that can be mined from different datasets. Moreover, the connection amongst the observable phenomena and the long-term dynamics of such systems is also discussed.

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Updated study of the quintuple system V994 Herculis

Cited by 22 publications

References 14 publications

TIC 278956474: Two Close Binaries in One Young Quadruple System Identified by TESS

TIC 278956474: Two Close Binaries in One Young Quadruple System Identified by TESS

Resonant capture in quadruple stellar systems

Eclipsing Binaries in Dynamically Interacting Close, Multiple Systems

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