Tidal interactions in star cluster simulations

Mardling, Rosemary A.; Aarseth, Sverre J.

doi:10.1046/j.1365-8711.2001.03974.x

Cited by 456 publications

(525 citation statements)

References 37 publications

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“…A typical ratio of a 3 /a 2 required for dynamical stability in our simulations is ∼ 6 (assuming the criterion of Mardling & Aarseth 2001). This implies an upper limit on a 2 of ∼ 10 3 /6 AU ≈ 167 AU, and which is indeed roughly consistent with the upper limit a 2 10 2 AU found in the simulations.…”

Section: Orbital Properties Of the Stellar Triple Arranged By Outcomementioning

confidence: 89%

“…In the case of '2+2' systems, sampled orbital combinations were rejected if a 3 /a 2 was smaller than the critical value for dynamical stability according to the criterion of Mardling & Aarseth (2001). Here, we treated orbits 2 and 3 as an isolated triple system with the mass of the 'tertiary' given by m 0 + m 1 , which is likely a good approximation given the small relative mass of the planet.…”

Section: Initial Conditionsmentioning

confidence: 99%

“…Similarly, in the case of '3+1' systems, stability of orbits 2 and 3 was assessed using the criterion of Mardling & Aarseth (2001), treating orbit 1 as a point mass with mass m 0 +m 1 . For the planetary orbit, we again applied the criterion of Holman & Wiegert (1999), this time treating orbits 1 and 2 as an isolated system (i.e.…”

Section: Initial Conditionsmentioning

confidence: 99%

“…(v) The stellar orbits became dynamically unstable according to the criterion of Mardling & Aarseth (2001). Note that this only applies to stellar triples.…”

Section: Stopping Conditionsmentioning

confidence: 99%

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On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Hamers

2017

Mon. Not. R. Astron. Soc.

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Hot Jupiters (HJs) are Jupiter-like planets orbiting their host star in tight orbits of a few days. They are commonly believed not to have formed in situ, requiring inwards migration towards the host star. One of the proposed migration scenarios is secular high-eccentricity or high-e migration, in which the orbit of the planet is perturbed to high eccentricity by secular processes, triggering strong tidal evolution and orbital migration. Previous theoretical studies have considered secular excitation in stellar binaries. Recently, a number of HJs have been observed in stellar triple systems. In the latter, the secular dynamics are much richer compared to stellar binaries, and HJs could potentially be formed more efficiently. Here, we investigate this possibility by modeling the secular dynamical and tidal evolution of planets in two hierarchical configurations in stellar triple systems. We find that the HJ formation efficiency is higher compared to stellar binaries, but only by at most a few tens of per cent. The orbital properties of the HJs formed in the simulations are very similar to HJs formed in stellar binaries, and similarly to studies of the latter we find no significant number of warm Jupiters. HJs are only formed in our simulations for triples with specific orbital configurations, and our constraints are approximately consistent with current observations. In future, this allows to rule out high-e migration in stellar triples if a HJ is detected in a triple grossly violating these constraints.

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Section: Orbital Properties Of the Stellar Triple Arranged By Outcomementioning

confidence: 89%

Section: Initial Conditionsmentioning

confidence: 99%

Section: Initial Conditionsmentioning

confidence: 99%

“…(v) The stellar orbits became dynamically unstable according to the criterion of Mardling & Aarseth (2001). Note that this only applies to stellar triples.…”

Section: Stopping Conditionsmentioning

confidence: 99%

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On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Hamers

2017

Mon. Not. R. Astron. Soc.

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“…These comprise from d5% up to 30% of all events in [BH, BH] binaries. The question is now whether the triplet that forms is long-term stable or short-term stable, i.e., destined to lose one of its components after a few outer-orbital times (Mardling & Aarseth 2001).…”

Section: Exotic End Statesmentioning

confidence: 99%

Probing the Presence of a Single or Binary Black Hole in the Globular Cluster NGC 6752 with Pulsar Dynamics

Colpi

Mapelli

Possenti

2003

ApJ

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The five millisecond pulsars that inhabit NGC 6752 display locations or accelerations that are quite unusual compared to all other known pulsars in globular clusters. In particular, PSR A, a binary pulsar, lives in the cluster halo, while PSR B and PSR E, located in the core, show remarkably high negative spin derivatives. This suggests that some uncommon dynamical process is at play in the cluster core, which we attribute to the presence of a massive perturber. Here we investigate whether a single intermediate-mass black hole, lying on the extrapolation of the mass M BH versus relation observed in galaxy spheroids, or a less massive binary black hole could play the requested role. To this purpose we simulated binary-binary encounters involving PSR A, its companion star, and the black hole(s). A stellar-mass binary black hole of (50 M ; 10 M ) can impart the right thrust to propel PSR A into the halo during a flyby. The flyby is gentle and does not alter the internal properties of the binary pulsar. An intermediate-mass binary black hole of (200 M ; 10 M ) tends to impart a recoil speed larger than the escape speed: it can release PSR A on the right orbit if its separation is wide. A single intermediate-mass black hole of mass M BH e500 M may have ejected PSR A at the periphery of NGC 6752 in a close dynamical encounter involving the binary pulsar, the black hole, and a star belonging to its cusp. The encounter gives correct speeds but alters significantly the eccentricity of the impinging binary, so that it must occur before the neutron star of PSR A is recycled via accretion torque. The influence of an intermediate-mass binary black hole on the acceleration of the two core pulsars is studied, and the ejection of stars by the binary is briefly explored. In inspecting our close four-body encounters, we have found that a single or binary black hole may attract on a long-term stable orbit a millisecond pulsar. Timing measurements on the captured '' satellite '' pulsar, either a member of a hierarchical triple or a member of the cusp, could unambiguously unveil the presence of a black hole(s) in the core of a globular cluster.

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