The first study of four doubly eclipsing systems

Zasche, P.; Henzl, Z.; Kára, Jan

doi:10.1051/0004-6361/202142771

Cited by 4 publications

(1 citation statement)

References 30 publications

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“…the continuous light curves of TESS), multiple epochs sample each individual eclipse and the individual eclipses are easy to identify. This makes the identification of double eclipsing binaries relatively straightforward (Zasche et al 2019(Zasche et al , 2022aKostov et al 2022). However, if a light curve is sparsely sampled (the typical time between observations is much larger than the duration of an eclipse), individual eclipses are sampled by a few or just a single epoch only and the light curve needs to be phase-folded in order to identify eclipses.…”

Section: Methodsmentioning

confidence: 99%

A systematic search for double eclipsing binaries in Zwicky Transient Facility data

Vaessen,

van Roestel

2024

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Double eclipsing binaries are gravitationally bound quadruple systems in a `2+2' configuration where both of the binaries are eclipsing. These systems are interesting objects to better understand stellar formation, to investigate the dynamical interaction between the two binary systems, or to study certain stages of stellar evolution, such as common-envelope events or Type Ia Supernovae. With this work, we aim to determine if double eclipsing binaries can be found using ZTF data and what the difficulties are in doing so. Secondly, we aim to significantly increase the number of known double eclipsing systems and determine how this sample differs from samples of double eclipsing binaries found with other telescopes. We developed a new method to systematically search for double eclipsing binaries in sparsely sampled light curves. For this we used box-least-squares (BLS) to search for the period of the first binary in the system. We then removed that signal from the light curves, and searched the residual light curve again with BLS to find the second period. We applied this method to ZTF light curves of 575\,526 eclipsing binaries known in the Gaia eclipsing binary catalogue. We report the discovery of 198 new double eclipsing binary systems. The shortest and longest orbital periods of the newly detected systems are 0.11 days to 323 days respectively. We successfully implemented a method that systematically searches for double eclipsing binary systems in sparsely sampled data. In total 198 new double eclipsing binary systems have been found in 575\,526 light curves (approx 0.034$<!PCT!>$). The ZTF sample typically contains more short period binaries compared to the TESS sample, but is also able to find systems with longer periods than what is currently known. We expect that at least three to four times more quadruples can be found by applying this method to all ZTF stellar light curves, by increasing the number of data points as a result of longer observations, and by implementing an automatic detection mechanism that replaces visual inspection.

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Section: Methodsmentioning

confidence: 99%

A systematic search for double eclipsing binaries in Zwicky Transient Facility data

Vaessen,

van Roestel

2024

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The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Pejcha

Cagaš

Landri

et al. 2022

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CzeV343 (=V849 Aur) was previously identified as a candidate double eclipsing binary (2+2 quadruple), where the orbital periods of the two eclipsing binaries (P A ≈ 1.2 days and P B ≈ 0.8 days) lie very close to a 3:2 resonance. Here, we analyze 11 years of ground-based photometry, four sectors of Transiting Exoplanet Survey Satellite (TESS) 2-minute and full-frame photometry, and two optical spectra. We construct a global model of our photometry, including apsidal motion of binary A and the light-travel time effect (LTTE) of the mutual outer orbit, and explore the parameter space with Markov Chain Monte Carlo. We estimate component masses for binary A (1.8 + 1.3 M ) and binary B (1.4 + 1.2 M ). We identify the pseudo-synchronous rotation signal of binary A in TESS photometry. We detect apsidal motion in binary A with a period of about 33 years, which is fully explained by tidal and rotational contributions of stars aligned with the orbit. The mutual orbit has a period of about 1450 days and an eccentricity of about 0.7. The LTTE amplitude is small, which points to low inclination of the outer orbit and a high degree of misalignment with the inner orbits. We find that when apsidal motion and the mutual orbit are taken into account, the orbital period resonance is exact to within 10 −5 cycles/day. Many properties of CzeV343 are not compatible with requirements of the 3:2 resonance capture theory for coplanar orbits. Future evolution of CzeV343 can lead to mergers, triple common envelope, double white dwarf binaries, or a Type Ia supernova. More complex evolutionary pathways will likely arise from dynamical instability caused by orbital expansion when either of thez binaries undergoes mass transfer. This instability has not been explored so far in 2+2 quadruples.

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Detection of seven 2+2 doubly eclipsing quadruple systems

Zasche¹,

Henzl²,

Mašek³

et al. 2023

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In this work, we study a heterogeneous group of seven stellar systems for the first time. Despite their different distances or spectral types, all of them belong to a very rare group of quadruple systems of 2+2 architecture, where both of the inner pairs harbor eclipsing binaries. These systems are: ASASSN-V J102911.57−522413.6 (inner periods 0.57272, and 3.79027 days), V1037 Her (0.78758 and 5.80348 days), WISE J181904.2+241243 (0.36713 and 0.41942 days), V2894 Cyg (2.57434 and 1.30579 days), NSVS 5725040 (1.79368 and 0.76794 days), WISE J210230.8+610816 (1.84324 and 0.57159 days), and ZTF J220518.78+592642.1 (2.79572 and 3.34615 days). Their outer mutual periods are: 9.3, 25.4, 18.7, 27.5, 2.6, 2.2, and 14.0 yr, respectively. These outer periodicities were derived using longer time span of photometric observations of these systems and analysing their period changes of both inner pairs via ETVs (eclipse-timing variations). Most of these studied systems are detached, as evidenced by the proper modelling of their light curves. A few of them show significant eccentric orbits with apsidal motion (e.g., V2894 Cyg, and NSVS 5725040). Further spectroscopic follow-up observations would offer a better characterization of the component star’s parameters (for e.g., NSVS 5725040), as well as a potential interferometric detection of the systems as real doubles on their mutual orbits (for e.g., V1037 Her). A rather interesting excess of systems close to a 3:2 mean motion resonance is seen only for early spectral-type stars with higher temperatures.

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The first study of four doubly eclipsing systems

Cited by 4 publications

References 30 publications

A systematic search for double eclipsing binaries in Zwicky Transient Facility data

A systematic search for double eclipsing binaries in Zwicky Transient Facility data

The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Detection of seven 2+2 doubly eclipsing quadruple systems

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