CzeV1731: The unique doubly eclipsing quadruple system

Zasche, P.; Henzl, Z.; Lehmann, H.; Pepper, Joshua; Powell, Brian P.; Kostov, Veselin B.; Barclay, Thomas; Wolf, M.; Kučáková, H.; Uhlàř, R.; Mašek, M.; Palafouta, S.; Gazeas, K.; Stassun, Keivan G.; Gaudi, B. Scott; Rodriguez, Joseph E.; Stevens, Daniel J.

doi:10.1051/0004-6361/202038656

Cited by 5 publications

(3 citation statements)

References 23 publications

(15 reference statements)

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“…The target presented here, TIC 454140642, exhibits the typical 2+2 hierarchy for quadruple systems, illustrated in Fig. 1, and joins the small number of such confirmed, well-characterized systems -VW LMi (Pribulla et al 2008), V994 Her (Zasche & Uhlař 2016), V482 Per (Torres et al 2017), EPIC 220204960 (Rappaport et al 2017, EPIC 219217635 (Borkovits et al 2018), CzeV1731 (Zasche et al 2020), TIC 278956474 (Rowden et al 2020), and BG Ind (Borkovits et al 2021).…”

Section: Introductionsupporting

confidence: 64%

TIC 454140642: A Compact, Coplanar, Quadruple-lined Quadruple Star System Consisting of Two Eclipsing Binaries

Kostov

Powell

Torres

et al. 2021

ApJ

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Section: Introductionsupporting

confidence: 64%

TIC 454140642: A Compact, Coplanar, Quadruple-lined Quadruple Star System Consisting of Two Eclipsing Binaries

Kostov

Powell

Torres

et al. 2021

ApJ

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“…The long-term evolution of both A and B orbits can be studied using the eclipse timing data (so-called ETV analysis, or the O − C diagram analysis). We used the same approach in our former analysis of doubly eclipsing systems CzeV1731 (Zasche et al 2020), TIC 168789840 (Powell et al 2021), or all systems in Zasche et al (2019). Such a method is very powerful and effective when good data are available, adequately distributed in time, and well covered for both A and B binaries.…”

Section: )mentioning

confidence: 99%

The first study of four doubly eclipsing systems

Zasche

Henzl

Kára

2022

A&A

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We present the discovery and the very first analysis of four stellar systems showing two periods of eclipses, that are the objects classified as doubly eclipsing systems. Some of them were proved to orbit each other thanks to their eclipse-timing-variations (ETVs) of both pairs, hence they really constitute rare quadruples with two eclipsing pairs. Some of them do not, as we are still waiting for more data to detect their mutual movement. Their light curves and period changes were analysed. All of them are detached and near-contact, but none of them contact; moreover, to our knowledge none of these stars can be considered as blend of two spatially unresolved close components on the sky. These systems are CzeV2647 (0.5723296 + 0.9637074 days), proved to orbit with 4.5-year periodicity; CzeV1645 (1.0944877 + 1.6594641 days), with a rather questionable detection of ETV; CzeV3436 (0.6836870 + 0.3833930 days); and, finally, OGLE SMC-ECL-1758 (0.9291925 + 3.7350826 days), proved to move on its 30-year orbit. Even more surprising is the fact that most of these systems show the ratio of their two orbital periods close to coupling near some resonant values of small integers, namely CzeV2647, with only 1% from 3:5 resonance, CzeV1645 1% from 2:3 resonance, and OGLE SMC-ECL-1758 with only 0.49% from 1:4 resonance. The nature of these near-resonant states still remains a mystery.

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“…For some objects, it was possible to constrain the mutual orbit with the light travel time effect (LTTE) or with dynam-Full Table B.1 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/ ical perturbations to the inner orbits. For example, Zasche et al (2020) estimated an outer orbital period in CzeV1731 to about 34 years. Most DEBs characterized so far are compatible with aligned inner and outer orbits.…”

Section: Introductionmentioning

confidence: 99%

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

Pejcha

Cagaš

Landri

et al. 2022

A&A

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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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CzeV1731: The unique doubly eclipsing quadruple system

Cited by 5 publications

References 23 publications

TIC 454140642: A Compact, Coplanar, Quadruple-lined Quadruple Star System Consisting of Two Eclipsing Binaries

TIC 454140642: A Compact, Coplanar, Quadruple-lined Quadruple Star System Consisting of Two Eclipsing Binaries

The first study of four doubly eclipsing systems

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

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