Internal Dynamics of Globular Clusters

Meylan, G.

doi:10.1142/9789812793621_0004

Cited by 21 publications

(37 citation statements)

References 629 publications

(967 reference statements)

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“…Accessible descriptions of globular cluster evolution are given in Hut et al [241], Meylan and Heggie [326] and Meylan [325] and have also been the subject of several texts (e.g., Spitzer [443] and Heggie and Hut [199]). Here we merely outline some of the more important aspects of globular cluster evolution.…”

Section: Globular Clustersmentioning

confidence: 99%

“…Review articles of Meylan and Heggie [326] and Meylan [325] also provide a comprehensive look at the internal dynamics of globular clusters. Although our focus is mainly on the Galactic globular cluster system, the physics of globular cluster systems associated with other galaxies is well covered in the review article by Harris [192] as well as his lecture notes from the Saas-Fee course on star clusters [65].…”

Section: Introductionmentioning

confidence: 99%

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Relativistic Binaries in Globular Clusters

Benacquista¹,

Downing

2013

Living Rev. Relativ.

198

129

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Galactic globular clusters are old, dense star systems typically containing 104–106 stars. As an old population of stars, globular clusters contain many collapsed and degenerate objects. As a dense population of stars, globular clusters are the scene of many interesting close dynamical interactions between stars. These dynamical interactions can alter the evolution of individual stars and can produce tight binary systems containing one or two compact objects. In this review, we discuss theoretical models of globular cluster evolution and binary evolution, techniques for simulating this evolution that leads to relativistic binaries, and current and possible future observational evidence for this population. Our discussion of globular cluster evolution will focus on the processes that boost the production of tight binary systems and the subsequent interaction of these binaries that can alter the properties of both bodies and can lead to exotic objects. Direct N-body integrations and Fokker-Planck simulations of the evolution of globular clusters that incorporate tidal interactions and lead to predictions of relativistic binary populations are also discussed. We discuss the current observational evidence for cataclysmic variables, millisecond pulsars, and low-mass X-ray binaries as well as possible future detection of relativistic binaries with gravitational radiation.

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Section: Globular Clustersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Relativistic Binaries in Globular Clusters

Benacquista¹,

Downing

2013

Living Rev. Relativ.

198

129

View full text Add to dashboard Cite

show abstract

“…An overview of the evolution of globular clusters can be found in Hut et al [116], Meylan and Heggie [157], and Meylan [156]. We summarize here the aspects of globular cluster evolution that are relevant to the formation and concentration of relativistic binaries.…”

Section: Globular Clustersmentioning

confidence: 99%

“…Review articles of Meylan and Heggie [157] and Meylan [156] also provide a comprehensive look at the internal dynamics of globular clusters. Although our focus is solely on the Galactic globular cluster system, the physics of globular cluster systems associated with other galaxies is well covered in the review article by Harris [94] as well as his lecture notes from the Saas-Fee course on star clusters [29].…”

Section: Introductionmentioning

confidence: 99%

Relativistic Binaries in Globular Clusters

Benacquista¹

2006

Living Rev. Relativ.

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The galactic population of globular clusters are old, dense star systems, with a typical cluster containing 104–107 stars. As an old population of stars, globular clusters contain many collapsed and degenerate objects. As a dense population of stars, globular clusters are the scene of many interesting close dynamical interactions between stars. These dynamical interactions can alter the evolution of individual stars and can produce tight binary systems containing one or two compact objects. In this review, we discuss the theoretical models of globular cluster evolution and binary evolution, techniques for simulating this evolution which lead to relativistic binaries, and current and possible future observational evidence for this population. Globular cluster evolution will focus on the properties that boost the production of hard binary systems and on the tidal interactions of the galaxy with the cluster, which tend to alter the structure of the globular cluster with time. The interaction of the components of hard binary systems alters the evolution of both bodies and can lead to exotic objects. Direct N-body integrations and Fokker-Planck simulations of the evolution of globular clusters that incorporate tidal interactions and lead to predictions of relativistic binary populations are also discussed. We discuss the current observational evidence for cataclysmic variables, millisecond pulsars, and low-mass X-ray binaries as well as possible future detection of relativistic binaries with gravitational radiation.

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“…Inevitable presence of dynamic drag inside gaseous objects (including GC, see Meylan and Heggie 1997) and other forms of friction forces acting on a test body inside mass M has surprisingly only a minor effect on resulting dynamics, at least in the framework of presented model. Drag suppress amplitude of oscillations and delay onset of the instability.…”

Section: Numerical Verification Of the Instability And The Long-term mentioning

confidence: 92%

Generalized Three-body Problem and the Instability of the Core-halo Objects in Binary Systems

Odrzywołek¹

2015

Acta Phys. Pol. B

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Goal of the presented research is to construct simplified model of the core-halo structures in binary systems. Examples are provided by Thorne-Zytkov objects, hot Jupiters, protoplanets with large moons, red supergiants in binaries and globular clusters with central black hole. Instability criteria due to resonance between internal and orbital frequencies in such a systems has been derived. To achieve assumed goals, generalized planar circular restricted three body problem is investigated with one of the point masses, M , replaced with spherical body of finite size. Mechanical system under consideration includes two large masses m and M and the test body with small mass µ. Mass µ, initially, is placed in the geometric center of mass M , and shares its orbital motion. Only gravitational interactions are considered, and non-point mass M is assumed to be rigid with rotational degrees of freedom neglected. Equations of motion are presented, and linear instability criteria are derived using quantifier elimination.Motion of the test mass µ is shown to be unstable due to resonance between orbital and internal frequencies if, where ρ is the central density of mass M , and d distance between masses m and M (circular orbit diameter). In the framework of model, the central mass µ can be ejected if resonance conditions are met during the evolution of the system. The above result is important for core-collapse supernova theory, with mass µ identified with helium core of the exploding massive star. The instability cause off-center supernova "ignition" relative to the center-of-mass of the hydrogen envelope. The instability is also inevitable during protoplanet growth, with hypothetical ejection of the rocky core from gas giants and formation of the "puffy planets" due to resonance with orbital frequency. Hypothetical central intermediate black holes of the globular clusters are also in unstable position with respect to perturbations caused by the Galaxy. For sake of curiosity I note, that the Earth-Moon, and the Earth-Sun systems are stable in the above sense, with test body µ being the artificial black hole created in the failed high-energy physics experiment.

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Internal Dynamics of Globular Clusters

Cited by 21 publications

References 629 publications

Relativistic Binaries in Globular Clusters

Relativistic Binaries in Globular Clusters

Relativistic Binaries in Globular Clusters

Generalized Three-body Problem and the Instability of the Core-halo Objects in Binary Systems

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