VW LMi: tightest quadruple system known. Light-time effect and possible secular changes of orbits<sup>★</sup>

Pribulla, T.; Baludansky, D.; Dubovský, Pavol A.; Kudzej, Igor; Parimucha, Š.; Siwak, M.; Vaňko, M.

doi:10.1111/j.1365-2966.2008.13781.x

Cited by 27 publications

(30 citation statements)

References 24 publications

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“…We reproduced the stellar and orbital parameters derived by Casey et al (1998) based on the 2009 VYSOS6 data (Fig. 1) using the methods of Pribulla et al (2008). It can be noticed that the secondary minimum at a phase of ≈ 0.5 already becomes more pronounced in the R and I bands, compared to the B and V bands.…”

Section: Overviewmentioning

confidence: 82%

Multiwavelength Photometry of the Young Intermediate Mass Eclipsing Binary TY CrA

Eiff¹,

Vaňko

Pribulla

et al. 2011

Proc. IAU

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Abstract.One of the handful of known PMS eclipsing binaries is a component of the spectroscopic triple TY CrA. Its secondary component is particularly interesting since it is a star of relatively high mass (1.64 M ) which is still on the pre-main sequence. The eclipsing binary was analyzed in the optical wavelength range ∼10 years ago, however, the crucial secondary eclipse minimum is very shallow. Therefore, we are obtaining new photometry in both optical and near-IR bands. We present first observations in (BVRI) which show that the secondary eclipse depth increases to about 0.1 mag in the I band. The increased eclipse depth with respect to other bands will help to better determine the colours and dimensions of the system. Furthermore, we show and discuss first near-IR observations of the primary eclipse. In addition to the light curves we are obtaining radial velocities in order to pin down the orbital parameters of the triple. Our first observations agree with the orbital parameters derived ∼10 years ago.

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Section: Overviewmentioning

confidence: 82%

Multiwavelength Photometry of the Young Intermediate Mass Eclipsing Binary TY CrA

Eiff¹,

Vaňko

Pribulla

et al. 2011

Proc. IAU

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“…On the other hand, the RV and timing-variability analysis of Pribulla et al (2008) showed that except the dynamically-induced apsidal motion in the DNEB, no perturbations could be detected in 10 years of observations. The analysis showed that the inclinations of the inner and outer orbits are similar.…”

Section: Perturbations Of Orbits In Multiple Systemsmentioning

confidence: 90%

“…The binaries revolve in a tight mutual outer orbit with P1234 = 355 days. Later, Pribulla et al (2008) determined the masses of all four components by simultaneous modelling of 4 radial-velocity (RV) curves and timing variability of the CEB caused by the light-time effect (LiTE) in the outer mu- Table 1. Overview of identifications and basic parameters of VW LMi.…”

Section: Introductionmentioning

confidence: 99%

Secular changes in the orbits of the quadruple system VW LMi

Pribulla

Puha

Borkovits

et al. 2020

Monthly Notices of the Royal Astronomical Society

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VW LMi is the tightest known quadruple system with 2+2 hierarchy. It consists of a W UMa-type eclipsing binary (P 12 = 0.47755 days) and another detached non-eclipsing binary (P 34 = 7.93 days) orbiting around a common center of mass in about P 1234 = 355 days. We present new observations of the system extending the time baseline to study long-term perturbations in the system and to improve orbital elements. The multi-dataset modeling of the system (4 radial-velocity curves for the components and the timing data) clearly showed an apsidal motion in the non-eclipsing binary at a rate of 4.6 degrees/yr, but no other perturbations. This is consistent with the nearly co-planarity of the outer, 355-day orbit, and the 7.93-day orbit of the non-eclipsing binary. Extensive N-body simulations enabled us to constrain the mutual inclination of the non-eclipsing binary and the outer orbits to j 34−1234 < 10 degrees.

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“…During the DDO survey, we detected not only many triple systems: Some complex, close quadruple systems were observed as well. Among them, worth pointing out is the very interesting system of VW LMi with the outer orbit of 355 days [34,49].…”

Section: Triple Systemsmentioning

confidence: 99%

Contact Binaries: The Current State

Ruciński¹

2010

AIP Conference Proceedings

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Lucy's model of contact binaries has been serving well since its development in 1968 as an excellent conceptual framework for internal structure and evolution studies of the W UMa type stars. Its over-constrained structural demands were recognized early, but -from the observational point of view -it was particularly appealing in its ability to explain W UMa-type binary light curves. Large numbers of photometric light curves of W UMa type binaries have been solved for geometrical parameters utilizing the clarity and simplicity of Lucy's model to the point of frequent over-interpretation of the meager lightcurve information content. Many, single, photometric solutions do not translate into a satisfactory understanding of these binaries. As the David Dunlap Observatory radial velocity program of bright, close binary stars (conducted in the last 10 years before the observatory closure in 2008) has shown, there are problems when spectroscopic results are confronted with light-curve solutions: Very frequently, the crucial parameter of the mass-ratio determined spectroscopically is entirely different from its photometric analogue (i.e. the one determined assuming a strict adherence to the Lucy's model), the third star incidence is high (which makes light curve solutions difficult, if not entirely wrong, even for totally eclipsing systems) and -last but not least -the model has serious difficulties for the best observed case of the crucially important, very low mass-ratio system AW UMa. One would argue that it is spectroscopy which gives correct results, but it requires access to large telescopes, extensive use of special techniques to analyze strongly blended and rotationally broadened spectra and is simply much harder to do than photometry. If the light curve solutions deceive us into believing in correctness of Lucy's contact-binary model and if only a fraction of (or none among) W UMa systems can be explained by that model, then the subject of contact binaries needs new ideas and new, mostly spectroscopic, high quality observations.

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VW LMi: tightest quadruple system known. Light-time effect and possible secular changes of orbits^★

Cited by 27 publications

References 24 publications

Multiwavelength Photometry of the Young Intermediate Mass Eclipsing Binary TY CrA

Multiwavelength Photometry of the Young Intermediate Mass Eclipsing Binary TY CrA

Secular changes in the orbits of the quadruple system VW LMi

Contact Binaries: The Current State

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VW LMi: tightest quadruple system known. Light-time effect and possible secular changes of orbits★

Cited by 27 publications

References 24 publications

Multiwavelength Photometry of the Young Intermediate Mass Eclipsing Binary TY CrA

Multiwavelength Photometry of the Young Intermediate Mass Eclipsing Binary TY CrA

Secular changes in the orbits of the quadruple system VW LMi

Contact Binaries: The Current State

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VW LMi: tightest quadruple system known. Light-time effect and possible secular changes of orbits^★