Problems of collisional stellar dynamics

Heggie, Douglas C.

doi:10.1142/9789814374774_0009

Cited by 3 publications

(2 citation statements)

References 92 publications

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“…For a comprehensive view on theoretical and computational aspects we refer the reader to the books by Heggie and Hut (2003), , Merritt (2013), and Portegies Zwart and McMillan (2018). Several recent review articles are also available on: the internal dynamics of star clusters (Vesperini 2010;Heggie 2011;McMillan 2015), young massive star clusters (Portegies Zwart et al 2010;Longmore et al 2014), multiple stellar populations in globular clusters (Bastian and Lardo 2017;Gratton et al 2012), star clusters in the landscape of galaxy formation and evolution (Renaud 2018;Kruijssen 2014), as well as the summary of a recent conference on the formation of globular clusters in a cosmological context (Forbes et al 2018).…”

Section: Introductionmentioning

confidence: 99%

A MODEST review

et al. 2018

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We present an account of the state of the art in the fields explored by the research community invested in "Modeling and Observing DEnse STellar systems". For this purpose, we take as a basis the activities of the MODEST-17 conference, which was held at Charles University, Prague, in September 2017. Reviewed topics include recent advances in fundamental stellar dynamics, numerical methods for the solution of the gravitational N-body problem, formation and evolution of young and old star clusters and galactic nuclei, their elusive stellar populations, planetary systems, and exotic compact objects, with timely attention to black holes of different classes of mass and their role as sources of gravitational waves.Such a breadth of topics reflects the growing role played by collisional stellar dynamics in numerous areas of modern astrophysics. Indeed, in the next decade many revolutionary instruments will enable the derivation of positions and velocities of individual stars in the Milky Way and its satellites, and will detect signals from a range of astrophysical sources in different portions of the electromagnetic and gravitational spectrum, with an unprecedented sensitivity. On the one hand, this wealth of data will allow us to address a number of long-standing open questions in star cluster studies; on the other hand, many unexpected properties of these systems will come to light, stimulating further progress of our understanding of their formation and evolution.

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Section: Introductionmentioning

confidence: 99%

A MODEST review

et al. 2018

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“…For a comprehensive view on theoretical and computational aspects we refer the reader to the books by Heggie and Hut (2003), , Merritt (2013), and Portegies Zwart and McMillan (2018). Several review articles are also available on: the internal dynamics of star clusters (Heggie, 2011;McMillan, 2015;Vesperini, 2010), young massive star clusters (Longmore et al, 2014;Portegies Zwart et al, 2010), multiple stellar populations in globular clusters (Bastian and Lardo, 2017;Gratton et al, 2012), star clusters in merging galaxies (Renaud, 2018), as well as the summary of a recent conference on the formation of globular clusters in a cosmological context (Forbes et al, 2018). [2] https://modest17.cuni.cz/ [3] The electronic version of the book of abstracts, which includes also almost all posters, is available at: https://modest17.cuni.cz/doc/modest17-boa.pdf 2 Stellar dynamics…”

Section: Introductionmentioning

confidence: 99%

A MODEST review

Varri,

Cai,

Concha-Ramírez

et al. 2018

Preprint

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We present an account of the state of the art in the fields explored by the research community invested in "Modeling and Observing DEnse STellar systems" . For this purpose, we take as a basis the activities of the MODEST-17 conference, which was held at Charles University, Prague, in September 2017. Reviewed topics include recent advances in fundamental stellar dynamics, numerical methods for the solution of the gravitational N -body problem, formation and evolution of young and old star clusters and galactic nuclei, their elusive stellar populations, planetary systems, and exotic compact objects, with timely attention to black holes of different classes of mass and their role as sources of gravitational waves.Such a breadth of topics reflects the growing role played by collisional stellar dynamics in numerous areas of modern astrophysics. Indeed, in the next decade many revolutionary instruments will enable the derivation of positions and velocities of individual stars in the Milky Way and its satellites, and will detect signals from a range of astrophysical sources in different portions of the electromagnetic and gravitational spectrum, with an unprecedented sensitivity. On the one hand, this wealth of data will allow us to address a number of long-standing open questions in star cluster studies; on the other hand, many unexpected properties of these systems will come to light, stimulating further progress of our understanding of their formation and evolution.

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Introducing a new multi-particle collision method for the evolution of dense stellar systems

Cintio

Pasquato

Simon-Petit

et al. 2022

A&A

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Context. In a previous paper we introduced a new method for simulating collisional gravitational N-body systems with linear time scaling on N, based on the multi-particle collision (MPC) approach. This allows us to easily simulate globular clusters with a realistic number of stellar particles (105 − 106) in a matter of hours on a typical workstation. Aims. We evolve star clusters containing up to 106 stars to core collapse and beyond. We quantify several aspects of core collapse over multiple realizations and different parameters while always resolving the cluster core with a realistic number of particles. Methods. We run a large set of N-body simulations with our new code MPCDSS. The cluster mass function is a pure power law with no stellar evolution, allowing us to clearly measure the effects of the mass spectrum on core collapse. Results. Leading up to core collapse, we find a power-law relation between the size of the core and the time left to core collapse. Our simulations thus confirm the theoretical self-similar contraction picture but with a dependence on the slope of the mass function. The time of core collapse has a non-monotonic dependence on the slope, which is well fitted by a parabola. This also holds for the depth of core collapse and for the dynamical friction timescale of heavy particles. Cluster density profiles at core collapse show a broken-power-law structure, suggesting that central cusps are a genuine feature of collapsed cores. The core bounces back after collapse, with visible fluctuations, and the inner density slope evolves to an asymptotic value. The presence of an intermediate-mass black hole inhibits core collapse, making it much shallower, irrespective of the mass-function slope. Conclusions. We confirm and expand on several predictions of star cluster evolution before, during, and after core collapse. Such predictions were based on theoretical calculations or small-size direct N-body simulations. Here we put them to the test in MPC simulations with a much larger number of particles, allowing us to resolve the collapsing core.

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Problems of collisional stellar dynamics

Cited by 3 publications

References 92 publications

A MODEST review

A MODEST review

A MODEST review

Introducing a new multi-particle collision method for the evolution of dense stellar systems

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