The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

Kovács, G.; Hartman, J. D.; Bakos, G. Á.

doi:10.1051/0004-6361/201936207

Cited by 12 publications

(8 citation statements)

References 62 publications

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“…Molnar et al (2017) suggested that the contact binary KIC 9832227 could be considered as a merger candidate based on a tentative exponential period decrease. However the system may not be a merger candidate according in a recent study (Socia et al 2018;Kovacs et al 2019). Pietrukowicz et al (2017) presented three potential merger candidates, EBs with relatively long orbital periods of more than P > 1.0 days and a relatively high decreasing period rate of more than Ṗ > −1.0 × 10 −5 day year −1 .…”

Section: Summary and Discussionmentioning

confidence: 99%

Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge

Hong,

Lee,

Park

et al. 2022

Preprint

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We present the orbital period variations of 14,127 contact eclipsing binaries (CEBs) based on the OGLE-III&IV observations in the Galactic bulge. New times of minimum lights for the CEBs were derived by binary modeling for the full seasonal light curves, which were made from survey observations at an interval of 1 year. The orbital period changes of the systems were classified based on the statistical inference, multiple-hypothesis testing error measure, and visual inspection of the eclipse timing diagrams. As the results, we identified 13,716 CEBs with a parabola, 307 CEBs with a sinusoid, and 104 CEBs with the two variations. The period distributions of the inner close binaries and the outer companions were in the ranges of 0.235 − 0.990 days and 5.0 − 14.0 years, respectively. In our sample of 13,820 CEBs showing a parabolic variation, the highest decreasing and increasing period rates were determined to be Ṗ = −1.38 ± 0.06 × 10 −5 day year −1 for OGLE-BLG-ECL-169991 and Ṗ = +8.99 ± 0.44 × 10 −6 day year −1 for OGLE-BLG-ECL-189805, respectively. The secular period change rates were distributed almost symmetrically around zero, and most of them lie within Ṗ = ±5.0 × 10 −6 day year −1 .

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Section: Summary and Discussionmentioning

confidence: 99%

Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge

Hong,

Lee,

Park

et al. 2022

Preprint

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“…The orbital shrinking was calculated to be so rapid, that KIC 9832227 was expected to become a red nova (and merge) within the next years (estimated to merge in 2022). Socia et al (2018) and Kovacs et al (2019) spotted a misinterpretation in archival data by Molnar's group and suggested that the system is not a red nova candidate. With a more robust and careful approach, the recent studies resulted in an contact configuration that includes a third component orbiting the contact binary, while the binary exhibits period decrease with a much lower rate (−0.1097(47) × 10 −7 d yr −1 ).…”

Section: The System Kic 9832227mentioning

confidence: 99%

CoBiToM Project -- I. Contact Binaries Towards Merging

Gazeas,

Loukaidou,

Niarchos

et al. 2021

Preprint

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Binary and multiple stellar systems are numerous in our solar neighborhood with 80 per cent of the solar-type stars being members of systems with high order multiplicity. The Contact Binaries T owards Merging (CoBiToM) Project is a programme that focuses on contact binaries and multiple stellar systems, as a key for understanding stellar nature. The goal is to investigate stellar coalescence and merging processes, as the final state of stellar evolution of low-mass contact binary systems. Obtaining observational data of approximately 100 eclipsing binaries and multiple systems and more than 400 archival systems, the programme aspires to give insights for their physical and orbital parameters and their temporal variations, e.g. the orbital period modulation, spot activity etc. Gravitational phenomena in multiple-star environments will be linked with stellar evolution. A comprehensive analysis will be conducted, in order to investigate the possibility of contact binaries to host planets, as well as the link between inflated hot Jupiters and stellar mergers. The innovation of CoBiToM Project is based on a multi-method approach and a detailed investigation, that will shed light for the first time on the origin of stellar mergers and rapidly rotating stars. In this work we describe the scientific rationale, the observing facilities to be used and the methods that will be followed to achieve the goals of CoBiToM Project and we present the first results as an example of the current research on evolution of contact binary systems.

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“…KIC 9832227 was originally reported to be a candidate for a future merger episode. Some of the ephemeris on which this claim was based have since been disproven (Socia et al 2018), with a more likely scenario that the system is a hierarchical triple (Kovacs et al 2019 (2017), light curve fit Figure 9. Time evolution of the orbital period and donor mass loss rate for v1309 Sco from data and RLOF modeling.…”

Section: N Decay -N Accel Planementioning

confidence: 99%

“…KIC 9832227 was originally reported to be a candidate for a future merger episode. Some of the ephemeris on which this claim was based have since been disproven (Socia et al 2018), with a more likely scenario that the system is a hierarchical triple (Kovacs et al 2019). How- RLOF models are initialized to match the first orbital period reported in Tylenda et al (2011), and to reach a separation of the donor's original radius at the time of the outburst's V-band peak.…”

Section: N Decay -N Accel Planementioning

confidence: 99%

Runaway Coalescence of Pre-common-envelope Stellar Binaries

MacLeod

Loeb

2020

ApJ

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We study the process of runaway, unstable Roche lobe overflow in coalescing binary systems and its dependence on the properties of the binary involved. We create three-dimensional hydrodynamic models of binary coalescences, and follow them through a phase of increasing Roche lobe overflow until the accretor is engulfed by the donor at the onset of a common envelope phase. In these models, we vary binary properties of mass ratio, donor structure and spin, and equation of state through the gas adiabatic index. We compare the numerical results to semi-analytic models of binary orbit evolution based on mass and angular momentum exchange between two point masses. Using our hydrodynamic simulations, we measure the key parameters: the donor mass loss rate and the angular momentum exchanged per unit mass loss from the donor. Using these calibrations, the semi-analytic model closely reproduces the escalating mass loss and runaway orbital decay observed in the hydrodynamic models.The semi-analytic model accurately reproduces the major differences in orbit evolution that arise with varying mass ratio and donor structure. We encapsulate the semi-analytic model in a publicly-released python package RLOF. We apply this model to the observed period decay and subsequent merger of the binary v1309 Sco, and find that it can simultaneously reproduce the observed orbital decay and time of outburst. We further demonstrate that there is a relationship between period derivative and second derivative that can be a useful metric for evaluating candidate merging binaries.

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The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

Cited by 12 publications

References 62 publications

Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge

Period Changes of 14,127 Contact Eclipsing Binaries in the Galactic Bulge

CoBiToM Project -- I. Contact Binaries Towards Merging

Runaway Coalescence of Pre-common-envelope Stellar Binaries

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