The Gravitational Million-Body Problem: A Multidisciplinary Approach to Star Cluster Dynamics

By F. Rasio. 2003

386 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics, Mathematical Physics

View Paper: https://www.semanticscholar.org/paper/e4ff1d00a16a320f1956455e6853ffab47e08014

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Citations in the corpus

Stellar Processes Near the Massive Black Hole in the Galactic Center (2005, background): “The dynamical processes in a gravitating stellar system canbe summarized by classifying stellar interactions by their distance scale (e.g. Binney & Tremaine1987; Heggie & Hut2003).”
Rates of compact object coalescences (2021, neutral): “retained black holes by a factor of a few (Heggie and Hut, 2003).”
Stellar Remnants in Galactic Nuclei: Mass Segregation (2006, methodology): “…‘‘luminosity’’ must be balanced by central energy production through disruptions and coalescences, in a manner similar to the hardening of binaries that powers the postcollapse expansion of globular clusters (Shapiro 1977; Inagaki & Lynden-Bell 1983; Heggie 1984; Heggie & Hut 2003, among others).”
Stellar-mass black holes in star clusters: implications for gravitational-wave radiation (2009, background): “The variation in a and e is random due to the stochastic nature of the encounters, but the binary hardens on average (see e.g. Heggie & Hut 2003, Chapters 19 and 21) and the overall hardening rate decreases with a.”
Multiple populations in globular clusters (2012, background): “In general, binaries having x > 1 (hard/close binaries) will, on average, become more bound as a result of interactions with single stars; for x < 1 (soft/wide binaries), binary/single-star interactions will generally lead to the disruption of the binary (see e.g., Heggie & Hut 2003 for a review).”
The dynamical state of stellar structure in star‐forming regions (2011, methodology): “For this, we use the relation between the virial and half-mass radius corresponding to a Plummer (1911) potential, which is given byrv = 1.3rh (e.g. Heggie & Hut 2003).”
The effects of fly‐bys on planetary systems (2010, background): “The fraction of stars, f enc, which encounter another star within a distance rmin, during the lifetime of a stellar cluster, τ , can be estimated as (Heggie & Hut 2003) fenc = ∫ τ 0 nσv dt, (10) where n is the number density, σ is the cross-section of the encounter and v is the velocity dispersion.”