V994 Herculis: a unique triply eclipsing sextuple star system

Zasche, P.; Borkovits, T.; Jayaraman, Rahul; Rappaport, S.; Brož, M.; Vokrouhlický, David; Bíró, I; Hegedüs, T.; Kiss, Z T; Uhlàř, R.; Schwengeler, Hans Martin; Pál, András; Mašek, M.; Howell, Steve B.; Dallaporta, S.; Munari, U.; Gagliano, R.; Jacobs, T.; Kristiansen, Martti H.; LaCourse, Daryll; Omohundro, Mark; Terentev, Ivan A.; Vanderburg, Andrew; Henzl, Z.; Powell, Brian P.; Kostov, Veselin B.

doi:10.1093/mnras/stad328

Cited by 6 publications

(2 citation statements)

References 36 publications

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“…The authors also reported updated masses of 3.01 ± 0.06 M ⊙ , 2.58 ± 0.05 M ⊙ , 1.84 ± 0.03 M ⊙ , and 1.93 ± 0.04 M ⊙ for the Aa, Ab, Ba, and Bb components, respectively. Ultimately, Zasche et al (2023) reported the discovery of a third set of eclipses in the TESS space-based and archival ground-based photometric data, which makes the system a triply eclipsing sextuple star system. The authors refined the orbital period of the A(Aa+Ab)-B(Ba+Bb) core system to 1062 ± 2 days and reported on its close to 3:2 mean motion resonance.…”

Section: Discussionmentioning

confidence: 99%

Observational mapping of the mass discrepancy in eclipsing binaries: Selection of the sample and its photometric and spectroscopic properties

Tkachenko,

Pavlovski,

Serebriakova

et al. 2024

A&A

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Eclipsing spectroscopic double-lined binaries are the prime source of precise and accurate measurements of masses and radii of stars. These measurements provide a stringent test for models of stellar evolution that are consistently reported to contain major shortcomings. The mass discrepancy observed for eclipsing spectroscopic double-lined binaries is one of the manifestations of the shortcomings in stellar evolution models. The problem reflects the inability of the models to accurately predict the effective temperature and surface gravity or luminosity of a star for a given mass. Our ultimate goal is to provide an observational mapping of the mass discrepancy and to propose a recipe for its solution. We initiated a spectroscopic monitoring campaign of 573 candidate eclipsing binaries classified as such based on their TESS light curves. In this work, we present a sub-sample of 83 systems for which orbital phase-resolved spectroscopy has been obtained and subsequently analysed with the methods of least-squares deconvolution and spectral disentangling. In addition, we employed TESS space-based light curves to provide photometric classification of the systems according to the type of their intrinsic variability. We confirmed 69 systems as being either spectroscopic binaries or higher-order multiple systems. We classified twelve stars as single, and we found two more objects that cannot be decisively classified as intrinsically variable single or binary stars. Moreover, 20 eclipsing binaries were found to contain at least one component that exhibits stellar oscillations. Spectroscopic orbital elements were obtained with the spectral disentangling method and reported for all systems classified as either SB1 or SB2. The sample presented in this work contains both detached and semi-detached systems and covers a range in the effective temperature and mass of the star of $ K and $M $ M$_ odot $, respectively. Based on a comparison of our own results with those published in the literature for well-studied systems, we conclude that there is an appreciable capability of the spectral disentangling method to deliver precise and accurate spectroscopic orbital elements from as few as six to eight orbital phase-resolved spectroscopic observations. Orbital solutions obtained this way are accurate enough to deliver age estimates with an accuracy of 10<!PCT!> or better for intermediate-mass F-type stars, an important resource for the calibration of stellar evolution models for future space-based missions, such as PLATO. Finally, despite the small size relative to the 573 systems that we will ultimately monitor spectroscopically, the sample presented in this work is already suitable to kick off observational mapping of the mass discrepancy in eclipsing binaries.

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Section: Discussionmentioning

confidence: 99%

Observational mapping of the mass discrepancy in eclipsing binaries: Selection of the sample and its photometric and spectroscopic properties

Tkachenko,

Pavlovski,

Serebriakova

et al. 2024

A&A

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“…More recently Zasche et al (2021) present an extensive sample of 162 early-type binary systems showing apsidal motion located in the Large Magellanic Cloud. This point is particularly important given that light curves and apsidal motion modelling were carried out for the first time for several systems simultaneously and in an environment with a chemical composition different from solar (for a more recent reference on apsidal motion measurements, see Zasche et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Theoretical tidal evolution constants for stellar models from the pre-main sequence to the white dwarf stage

Claret¹

2023

A&A

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Aims. One of the most reliable means of studying the stellar interior is through the apsidal motion in double line eclipsing binary systems since these systems present errors in masses, radii, and effective temperatures of only a few per cent. On the other hand, the theoretical values of the apsidal motion to be compared with the observed values depend on the stellar masses of the components and more strongly on their radii (fifth power). The main objective of this work is to make available grids of evolutionary stellar models that, in addition to the traditional parameters (e.g. age, mass, log g, Teff), also contain the necessary parameters for the theoretical study of apsidal motion and tidal evolution. This information is useful for the study of the apsidal motion in eclipsing binaries and their tidal evolution, and can also be used for the same purpose in exoplanetary systems. Methods. All models were computed using the MESA package. We consider core overshooting for models with masses ≥1.2M⊙. For the amount of core overshooting we adopted a recent relationship for mass × core overshooting. We adopted for the mixing-length parameter αMLT the value 1.84 (the solar-calibrated value). Mass loss was taken into account in two evolutionary phases. The models were followed from the pre-main sequence phase to the white dwarf (WD) stage. Results. The evolutionary models containing age, luminosity, log g, and Teff, as well as the first three harmonics of the internal stellar structure (k2, k3, and k4), the radius of gyration βy, and the dimensionless variable α, related to gravitational potential energy, are presented in 69 tables covering three chemical compositions: [Fe/H] = −0.50, 0.00, and 0.50. Additional models with different input physics are available.

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BU Canis Minoris – the most compact known flat doubly eclipsing quadruple system

Pribulla

Borkovits

Jayaraman

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We have found that the 2+2 quadruple star system BU CMi is currently the most compact quadruple system known, with an extremely short outer period of only 121 days. The previous record holder was TIC 219006972 (Kostov et al. 2023), with a period of 168 days. The quadruple nature of BU CMi was established by Volkov et al. (2021), but they misidentified the outer period as 6.6 years. BU CMi contains two eclipsing binaries (EBs), each with a period near 3 days, and a substantial eccentricity of ≃ 0.22. All four stars are within ∼0.1 M⊙ of 2.4 M⊙. Both binaries exhibit dynamically driven apsidal motion with fairly short apsidal periods of ≃ 30 years, thanks to the short outer orbital period. The outer period of 121 days is found both from the dynamical perturbations, with this period imprinted on the eclipse timing variations (ETV) curve of each EB by the other binary, and by modeling the complex line profiles in a collection of spectra. We find that the three orbital planes are all mutually aligned to within 1 degree, but the overall system has an inclination angle near 83.5○. We utilize a complex spectro-photodynamical analysis to compute and tabulate all the interesting stellar and orbital parameters of the system. Finally, we also find an unexpected dynamical perturbation on a timescale of several years whose origin we explore. This latter effect was misinterpreted by Volkov et al. (2021) and led them to conclude that the outer period was 6.6 years rather than the 121 days that we establish here.

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V994 Herculis: a unique triply eclipsing sextuple star system

Cited by 6 publications

References 36 publications

Observational mapping of the mass discrepancy in eclipsing binaries: Selection of the sample and its photometric and spectroscopic properties

Observational mapping of the mass discrepancy in eclipsing binaries: Selection of the sample and its photometric and spectroscopic properties

Theoretical tidal evolution constants for stellar models from the pre-main sequence to the white dwarf stage

BU Canis Minoris – the most compact known flat doubly eclipsing quadruple system

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