A simple random walk model explains the disruption process of hierarchical, Eccentric three-body systems

Mushkin, Jonathan; Katz, Boaz

doi:10.1093/mnras/staa2492

Cited by 16 publications

(29 citation statements)

References 17 publications

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“…For comparison, we computed the estimated disruption time of hierarchical triple systems following Mushkin & Katz (2020). Their estimate was derived after modeling the disruption of hierarchical 3-body systems by a random-walk process.…”

Section: Comparison With Mushkin and Katz Estimatementioning

confidence: 99%

“…Their estimate was derived after modeling the disruption of hierarchical 3-body systems by a random-walk process. Mushkin & Katz (2020) estimate the number of inner orbital periods N before a triple disrupts as…”

Section: Comparison With Mushkin and Katz Estimatementioning

confidence: 99%

“…Once a triple becomes unstable, the hierarchy is disrupted and the three bodies undergo violent and chaotic interactions, until one body is ejected and only a binary is left. The mechanisms by which some triples become unstable are still not fully understood (Toonen et al 2021;Hayashi et al 2022), yet many authors have tried to find analytic criteria to assess the stability of hierarchical triples (Mardling & Aarseth 2001;Mushkin & Katz 2020;Hayashi et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Predicting the Stability of Hierarchical Triple Systems with Convolutional Neural Networks

Lalande¹,

Trani²

2022

Preprint

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Understanding the long-term evolution of hierarchical triple systems is challenging due to its inherent chaotic nature, and it requires computationally expensive simulations. Here we propose a convolutional neural network model to predict the stability of hierarchical triples by looking at their evolution during the first 5 × 10 5 inner binary orbits. We employ the regularized few-body code tsunami to simulate 5 × 10 6 hierarchical triples, from which we generate a large training and test dataset. We develop twelve different network configurations that use different combinations of the triples' orbital elements and compare their performances. Our best model uses 6 time-series, namely, the semimajor axes ratio, the inner and outer eccentricities, the mutual inclination and the arguments of pericenter. This model achieves an area under the curve of over 95% and informs of the relevant parameters to study triple systems stability. All trained models are made publicly available, allowing to predict the stability of hierarchical triple systems 200 times faster than pure N -body methods.

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Section: Comparison With Mushkin and Katz Estimatementioning

confidence: 99%

Section: Comparison With Mushkin and Katz Estimatementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Predicting the Stability of Hierarchical Triple Systems with Convolutional Neural Networks

Lalande¹,

Trani²

2022

Preprint

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“…A higher eccentricity 1−e 2 < 0.05, (a 5% chance for a thermal distribution), would bring the D system to within 40 AU of the triple which is sufficiently close to allow energy exchange and stochastic semi-major axis evolution of the AB-D orbit over long times (e.g. Heggie 1975;Roy & Haddow 2003;Mushkin & Katz 2020). Without additional information it is thus not possible to determine the dynamical evolution of the system.…”

Section: Dynamical Processes In the Quintuple Systemmentioning

confidence: 99%

“…Alternatively, the entire system formed at a scale of ∼ 100 AU, and the D1-D2 binary dynamically migrated outwards due to the multi body gravitational interactions (e.g. Reipurth & Mikkola 2012;Mushkin & Katz 2020). The A-B system is separated by 24 AU, and therefore could have formed by disk fragmentation.…”

Section: How Did Hj2814 Form and How Will It Evolve?mentioning

confidence: 99%

Beyond binarity in A stars II. Disentangling the four stars in the vicinity of the triple HIP 87813 within the quintuple system HJ2814

Waisberg¹,

Klein²,

Katz³

2022

Preprint

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A-stars are the progenitors of about half of the white dwarfs (WDs) that currently exist. The connection between the multiplicity of A-stars and that of WDs is not known and both multiplicities are still poorly explored. We are in the process of obtaining tight constraints on a sample of 108 southern A-type stars that are part of the nearby VAST sample (De Rosa et al. 2014) by conducting near-infrared interferometric follow-up observations to the (twenty) stars among them which have large Gaia-Hipparcos accelerations. In this paper, we combine spectroscopy, adaptive optics imaging, NIR interferometry and Gaia-Hipparcos astrometry in order to disentangle the stars in the complicated HIP 87813 = HJ2814A system. We show that (i) a previously discovered faint star that is separated by 2" from the A star is actually a background source; (ii) the Gaia-Hipparcos acceleration is caused by a newly discovered 0.74M star that was missed in previous AO images and we solve for its P ≈ 60 yrs astrometric orbit; (iii) by combining previously obtained spectra we show that the A star has a very close 0.85M companion on a 13.4-day period orbit. The radial velocity curve combined with NIR interferometry constrains its orbit allowing Kozai-Lidov oscillations in the hierarchical triple to be ruled out. The system HJ2814 is one of only about fifteen known 5+ systems with an A star primary, and will result in a system of between two to five bound WDs within around a Hubble time.

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The mass-ratio distribution of tertiary-induced binary black hole mergers

Liu

Lai

2021

Monthly Notices of the Royal Astronomical Society

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Many proposed scenarios for black hole (BH) mergers involve a tertiary companion that induces von Zeipel-Lidov-Kozai (ZLK) eccentricity cycles in the inner binary. An attractive feature of such mechanisms is the enhanced merger probability when the octupole-order effects, also known as the eccentric Kozai mechanism, are important. This can be the case when the tertiary is of comparable mass to the binary components. Since the octupole strength [∝(1 − q)/(1 + q)] increases with decreasing binary mass ratio q, such ZLK-induced mergers favor binaries with smaller mass ratios. We use a combination of numerical and analytical approaches to fully characterize the octupole-enhanced binary BH mergers and provide semi-analytical criteria for efficiently calculating the strength of this enhancement. We show that for hierarchical triples with semi-major axis ratio a/aout ≳ 0.01–0.02, the binary merger fraction can increase by a large factor (up to ∼20) as q decreases from unity to 0.2. The resulting mass ratio distribution for merging binary BHs produced in this scenario is in tension with the observed distribution obtained by the LIGO/VIRGO collaboration, although significant uncertainties remain about the initial distribution of binary BH masses and mass ratios.

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A simple random walk model explains the disruption process of hierarchical, Eccentric three-body systems

Cited by 16 publications

References 17 publications

Predicting the Stability of Hierarchical Triple Systems with Convolutional Neural Networks

Predicting the Stability of Hierarchical Triple Systems with Convolutional Neural Networks

Beyond binarity in A stars II. Disentangling the four stars in the vicinity of the triple HIP 87813 within the quintuple system HJ2814

The mass-ratio distribution of tertiary-induced binary black hole mergers

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