Detection of seven 2+2 doubly eclipsing quadruple systems

Zasche, P.; Henzl, Z.; Mašek, M.; Uhlàř, R.; Kára, Jan; Merc, Jaroslav; Kučáková, H.

doi:10.1051/0004-6361/202346848

Cited by 5 publications

(1 citation statement)

References 33 publications

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“…Our next step is to model the high-quality TESS LCs of the eclipsing pair of TZ Boo by studying the O'Connell effect to improve the modeling of the system and shed more light on the surface activity of its components. To investigate the quadruple nature, we would have to model the second pair and study the ETV analysis signals of both pairs on the basis of archival photometry and new data, to confirm that both of them actually orbit a common barycenter (Zasche et al 2022(Zasche et al , 2023. In addition, supplementary methods based on astrometric, spectroscopic, or even interferometric observations and stability analysis should be used for cross-validation.…”

Section: Discussionmentioning

confidence: 99%

Investigating Period Variability Mechanisms in Eclipsing Binary Stars through Eclipsing Time Variation Analysis: A Case Study of TZ Bootis

Zervas,

Christopoulou,

Papageorgiou

2024

ApJ

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We present an effective strategy for extensive analysis of eclipsing time variations (ETVs) using modern and sophisticated optimization methods that comprise a set of tools to investigate period variability mechanisms in eclipsing binary stars such as the light-time effect, the Applegate mechanism, and mass transfer. We implement these methods for the first time assuming that the above mechanisms can act simultaneously in the puzzling W UMa–type binary star TZ Bootis by using archival and new TESS data spanning 75 yr and reexamining the up-to-date ETVs. Preliminary analysis of the TESS data revealed for the first time the presence of a second binary in agreement with previous spectroscopic data and astrometric results from Gaia DR3. We consider the most credible scenario for the ETV: two stellar circumbinary companions of minimum masses M 3 = 0.5 M ☉ and M 4 = 0.14 M ☉ in highly eccentric orbits e 3 = 0.70 and e 4 = 0.82 with periods P 3 = 38 yr and P 4 = 20 yr along with a 24 yr magnetic activity of the secondary component and a long-term period increase (dP/dt = 1.2 × 10−8 days yr−1), interpreted as a conservative mass transfer from the secondary to the primary component at a rate of dM 1/dt = 3.7 × 10−9 days yr−1. Further spectroscopic observations, analytical modeling of the second pair, and ETV analysis of both pairs are needed to investigate the quadruple nature of the system.

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Section: Discussionmentioning

confidence: 99%

Investigating Period Variability Mechanisms in Eclipsing Binary Stars through Eclipsing Time Variation Analysis: A Case Study of TZ Bootis

Zervas,

Christopoulou,

Papageorgiou

2024

ApJ

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A star under multiple influences

Kővári,

Strassmeier,

Kriskovics

et al. 2024

A&A

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Close binaries with magnetically active components are astrophysical laboratories for studying the effects of binarity on activity. Of particular interest are binary and multiple star systems that contain a solar-type active component with an internal structure similar to the Sun, allowing us to study how the dynamo of a solar-type star would work under different conditions. We have conducted a comprehensive investigation of V815\,Her using photometric and spectroscopic data to understand the origin of the activity and what influences it in the short and long term. Using space photometry we performed light curve modeling in order to derive astrophysical and orbital parameters for the eclipsing binary subsystem V815\,Her B. Using archival photometric data covering a century we carried out a time frequency analysis. Spectral synthesis was applied to determine the basic astrophysical parameters of the rapidly rotating primary using high-resolution STELLA spectra recorded in 2018. Photometric analysis of archived data revealed multiple cycles on timescales between sim 6.5 and sim 26 years, some of which may be harmonic. From TESS photometry we obtained an orbital solution for the V815\,Her B subsystem. By placing the primary component on the Hertzsprung$-$Russell-diagram, we could deduce an age of approx 30\,Myr, in line with the high Li-6707 abundance. The STELLA spectra covering the 200 day-long observing season enabled us to create 19 time-series Doppler images, which revealed a constantly changing spotted surface on a timescale of a few weeks. From the consecutive image pairs we built up the average cross-correlation function map to measure the surface differential rotation of the spotted star, from which we derive a weak solar-type surface shear. We found evidence that the V815\,Her B component previously apostrophized as a "third body" is actually an eclipsing close binary subsystem of two M dwarfs with a period of 0.5\,d, that is, V815\,Her is a 2+2 hierarchical quadruple system. The system is apparently young, only a few times ten million years old, consistent with the spotted primary V815\,Her Aa being a zero-age main-sequence star. Spot activity on the primary was found to be vivid. Fast starspot decay suggests that convective-turbulent erosion plays a more significant role in such a rapidly rotating star. The weak surface shear of V815\,Her Aa due to differential rotation is presumably confined by tidal forces of the close companion V815\,Her Ab. The slowly increasing photometric cycle of about 6.5 years on average is interpreted as a spot cycle of V815\,Her Aa, which is probably modulated by the eccentric wide orbit.

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Six new eccentric eclipsing systems with a third body

Zasche,

Henzl,

Wolf

2024

A&A

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We present the discovery of six new triple stellar system candidates composed of an inner eccentric-orbit eclipsing binary with an apsidal motion. These stars were studied using new, precise TESS light curves and a long-term collection of older photometric ground-based data. These data were used for the monitoring of ETVs (eclipse timing variations) and to detect the slow apsidal movements along with additional periodic signals. The systems analysed were ASASSN-V J012214.37+643943.3 (orbital period 2.01156 d, eccentricity 0.15, third body with 3.3 yr period); ASASSN-V J052227.78+345257.6 (2.42673 d, 0.35, 3.2 yr); ASASSN-V J203158.98+410731.4 (2.53109 d, 0.20, 2.7 yr); ASASSN-V J230945.10+605349.3 (2.08957 d, 0.18, 2.3 yr); ASASSN-V J231028.27+590841.8 (2.41767 d, 0.43, 4.9 yr); and NSV 14698 (3.30047 d, 0.147, 0.5 yr). In the system ASASSN-V J230945.10+605349.3, we detected a second eclipsing pair (per 2.99252 d) and found adequate ETV for the pair B, proving its 2+2 bound quadruple nature. All of these detected systems deserve special attention from long-term studies for their three-body dynamics since their outer orbital periods are not too long and because some dynamical effects should be detectable during the next decades. The system NSV 14698 especially seems to be the most interesting from the dynamical point of view due to it having the shortest outer period of the systems we studied, its fast apsidal motion, and its possible orbital changes during the whole 20th century.

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Detection of seven 2+2 doubly eclipsing quadruple systems

Cited by 5 publications

References 33 publications

Investigating Period Variability Mechanisms in Eclipsing Binary Stars through Eclipsing Time Variation Analysis: A Case Study of TZ Bootis

Investigating Period Variability Mechanisms in Eclipsing Binary Stars through Eclipsing Time Variation Analysis: A Case Study of TZ Bootis

A star under multiple influences

Six new eccentric eclipsing systems with a third body

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