Stellar Dynamics of Dense Stellar Systems

Hut, Piet

doi:10.1007/978-94-010-0864-8_4

Cited by 4 publications

(5 citation statements)

References 7 publications

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“…In the consumer sector, participation in synthetic worlds such as Second Life and World of Warcraft is estimated in the tens of millions (Hof, 2006;Nardi and Harris, 2006), while synthetic worlds are also emerging as interesting sites of experimentation among scientists, educators, and software teams (Bainbridge, 2007;Hut, 2008;Moore and Jackson, 2008;Schultze et al, 2008). In organizations, a number of dedicated synthetic worlds -such as Project Wonderland (from Sun Microsystems), ProtoSphere (from ProtonMedia), Olive (from Forterra Systems), and Qwaq (from Qwaq) -are being deployed within organizations for the purposes of supporting distributed collaboration, project management, and online learning and simulation.…”

Section: Nicole Enters the Project Wonderland Team Room And Sees Jon mentioning

confidence: 99%

The sociomateriality of organisational life: considering technology in management research

Orlikowski

2009

Cambridge Journal of Economics

692

491

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Section: Nicole Enters the Project Wonderland Team Room And Sees Jon mentioning

confidence: 99%

The sociomateriality of organisational life: considering technology in management research

Orlikowski

2009

Cambridge Journal of Economics

692

491

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“…In fact, the leading formation channel for a new binary from single stars is a three body encounter, which is proportional to ρ 3 s . ρ s is the number density of single stars and this density is expressed in physical units, appropriate for encounters, such that ρ= 1 corresponds to interparticle distances equal to the 90° turnaround impact parameter (Hut 1989). Therefore, in this units we have ρ s ≪ 1.…”

Section: Properties Of the Binary Populationmentioning

confidence: 99%

Star clusters with primordial binaries - III. Dynamical interaction between binaries and an intermediate-mass black hole

Trenti¹,

Ardi²,

Mineshige³

et al. 2007

Monthly Notices of the Royal Astronomical Society

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We present the first study of the dynamical evolution of an isolated star cluster that combines a significant population of primordial binaries with the presence of a central black hole. We use equal‐mass direct N‐body simulations, with N ranging from 4096 to 16 384 and a primordial binary ratio of 0–10 per cent; the black hole mass is about 1 per cent of the total mass of the cluster. The evolution of the binary population is strongly influenced by the presence of the black hole, which gives the cluster a large core with a central density cusp. Starting from a variety of initial conditions (Plummer and King models), we first encounter a phase, that last approximately 10 half‐mass relaxation times, in which binaries are disrupted faster compared to analogous simulations without a black hole. Subsequently, however, binary disruption slows down significantly due to the large core size. The dynamical interplay between the primordial binaries and the black hole thus introduces new features with respect to the scenarios investigated so far, where the influence of the black hole and of the binaries have been considered separately. A large core to half‐mass radius ratio appears to be a promising indirect evidence for the presence of an intermediate‐mass black hole in old globular clusters.

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“…In a model with primordial binaries, and are comparable, at least in order of magnitude, and it follows that . In other words, at a given density the rate of energy generation by primordial binaries far exceeds the rate of energy generation by binaries that first have to be formed at that density (Hut 1989).…”

Section: The Physical Picturementioning

confidence: 99%

Star clusters with primordial binaries - I. Dynamical evolution of isolated models

Heggie¹,

Trenti²,

Hut³

2006

Monthly Notices of the Royal Astronomical Society

104

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In order to interpret the results of complex realistic star cluster simulations, which rely on many simplifying approximations and assumptions, it is essential to study the behaviour of even more idealized models, which can highlight the essential physical effects and are amenable to more exact methods. With this aim, we present the results of N-body calculations of the evolution of equal-mass models, starting with primordial binary fractions of 0-100 per cent, with values of N ranging from 256 to 16 384. This allows us to extrapolate the main features of the evolution to systems comparable in particle number with globular clusters.In this range, we find that the steady-state 'deuterium main sequence' is characterized by a ratio of the core radius to half-mass radius that follows qualitatively the analytical estimate by Vesperini & Chernoff, although the N dependence is steeper than expected. Interestingly, for an initial binary fraction f greater than 10 per cent, the binary heating in the core during the post-collapse phase almost saturates (becoming nearly independent of f ), and so little variation in the structural properties is observed. Thus, although we observe a significantly lower binary abundance in the core with respect to the Fokker-Planck simulations by Gao et al., this is of little dynamical consequence.At variance with the study of Gao et al., we see no sign of gravothermal oscillations before 150 half-mass relaxation times. At later times, however, oscillations become prominent. We demonstrate the gravothermal nature of these oscillations.

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Stellar Dynamics of Dense Stellar Systems

Cited by 4 publications

References 7 publications

The sociomateriality of organisational life: considering technology in management research

The sociomateriality of organisational life: considering technology in management research

Star clusters with primordial binaries - III. Dynamical interaction between binaries and an intermediate-mass black hole

Star clusters with primordial binaries - I. Dynamical evolution of isolated models

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