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The dynamical evolution of massive black hole binaries i
An article or wearing apparel such as a belt buckle provided with an ornament on the front member and an indicator that is movable around the front member to any one of a plurality of predeterminedExpand
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The time-scale for core collapse in spherical star clusters
Abstract The collapse time for a cluster of equal-mass stars is usually stated to be either 330 central relaxation times (trc) or 12-19 half-mass relaxation times (trh). But the first of these timesExpand
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Models of Galaxies with Central Black Holes: Adiabatic Growth in Spherical Galaxies
We add black holes to nonrotating, spherical galaxy models, with the assumption that the black-hole growth is slow compared with the dynamical time but fast compared with the relaxation time. TheExpand
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The dynamical evolution of massive black hole binaries — II. Self-consistent N-body integrations
Abstract We use a hybrid N-body program to study the evolution of massive black hole binaries in the centers of galaxies, mainly to understand the factors affecting the binary eccentricity, theExpand
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Dynamical evolution of dense clusters of compact stars
Une simulation numerique de l'equation de Fokker-Planck est realisee pour etudier l'evolution dynamique des amas ouverts d'etoiles compactes (etoiles a neutrons et trous noirs). L'amas est considereExpand
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Dynamical evolution of elliptical galaxies with central singularities
We study the effect of a massive central singularity on the structure of a triaxial galaxy using N-body simulations. Starting from a single initial model, we grow black holes with various finalExpand
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A massive black hole at the centre of the quiescent galaxy M32
Massive black holes are thought to reside at the centres of many galaxies1,2, where they power quasars and active galactic nuclei. But most galaxies are quiescent, indicating that any central massiveExpand
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On the reliability of gravitational N-body integrations
In a self-gravitating system of point particles such as a spherical star cluster, small disturbances to an orbit grow exponentially on a time-scale comparable with the crossing time. The results ofExpand
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Dynamical limits on dark mass in the outer solar system
Simplified model solar systems with known observational errors are considered in conducting a dynamical search for dark mass and its minimum detectable amount, and in determining the significance ofExpand
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