Stability of hierarchical triples – I. Dependence on inner eccentricity and inclination

Mylläri, Aleksandr; Valtonen, M. J.; Pasechnik, A. V.; Mikkola, Seppo

doi:10.1093/mnras/sty237

Cited by 27 publications

(32 citation statements)

References 22 publications

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“…There are also other relevant criteria for stability of a hierarchical system[42,65,66]. Since the criteria are only necessary but not sufficient, the usefulness was questioned by Myllari et al[67]. Their study takes into account the effect of inner binary eccentricity and relative inclination.…”

mentioning

confidence: 99%

Gravitational waves from hierarchical triple systems with Kozai-Lidov oscillation

et al. 2020

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We study gravitational waves from a hierarchical three-body system up to first-order post-Newtonian approximation. Under certain conditions, the existence of a nearby third body can cause periodic exchange between eccentricity of an inner binary and relative inclination, known as Kozai-Lidov oscillations. We analyze features of the waveform from the inner binary system undergoing such oscillations. We find that variation caused due to the tertiary companion can be observed in the gravitational waveforms and energy spectra, which should be compared with those from isolated binaries and coplanar three-body system. The detections from future space-based interferometers will make possible the investigation of gravitational wave spectrum in mHz range and may fetch signals by sources addressed.

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confidence: 99%

Gravitational waves from hierarchical triple systems with Kozai-Lidov oscillation

et al. 2020

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“…We note these stability criteria deem a system unstable if at any point in time it will encounter instability and does not take timescale into consideration (e.g. Mylläri et al 2018). Thus, we stress that using these criteria underestimate the number of allowable systems within their lifetime.…”

Section: Applicationsmentioning

confidence: 99%

Supernovae Kicks in hierarchical triple systems

Naoz²

2019

Monthly Notices of the Royal Astronomical Society

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Most massive stars, if not all, are in binary configuration or higher multiples. These massive stars undergo supernova explosions and end their lives as either black holes or neutron stars. Recent observations have suggested that neutron stars and perhaps even black holes receive large velocity kicks at birth. Such natal kicks and the sudden mass loss can significantly alter the orbital configuration of the system. Here we derive general analytical expressions that describe the effects of natal kicks in binaries on hierarchical triple systems. We explore several proof-of-concept applications such as black hole and neutron stars binaries and X-ray binaries with either stellar or Supermassive Black Hole (SMBH) companions on a wide orbit. Kicks can disrupt the hierarchical configuration, although it is harder to escape the potential well of an SMBH. Some binary systems do escape the SMBH system resulting in hyper-velocity binary system. Furthermore, kicks can result in increasing or decreasing the orbital separations. Decreasing the orbital separation may have significant consequences in these astrophysical systems. For example, shrinking the separation post-supernova kick can lead to the shrinking of an inner compact binary that then may merge via Gravitational Wave (GW) emission. This process yields a supernova that is shortly followed by a possible GW-LIGO event. Interestingly, we find that the natal kick can result in shrinking the outer orbit, and the binary may cross the tertiary Roche limit, breaking up the inner binary. Thus, in the case of SMBH companion, this process can lead to either a tidal disruption event or a GW-LISA detection event (Extreme Mass ratio inspiral, EMRI) with a supernova precursor.

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“…where T is the period of the periodic orbit in the rotating frame and T 1 is the Keplerian period of the inner binary that corresponds to the osculating semimajor axis a 1 . For almost circular orbits a is equivalent to the pericenter distance, Q, used in various stability criteria (Mylläri et al, 2018). For µ = 0 we have the unperturbed problem and for µ = 1 it is m 0 = 1/3 and m 1 + m 2 = 2/3.…”

Section: Methodsmentioning

confidence: 99%

“…However due to the lack of sufficient number of constants of motion and the many parameters involved in the problem it is not possible to express an explicit condition for stability. A review on stability criteria of triple systems is given by Georgakarakos (2008) while a resent extended numerical studies on eccentric and inclined triple star systems is presented in Mylläri et al (2018) and He and Petrovich (2018).…”

Section: Introductionmentioning

confidence: 99%