Binary Stars and Globular Cluster Dynamics
arXiv:0710.3167 · doi:10.1017/S1743921308015676
Abstract
In this brief proceedings article I summarize the review talk I gave at the IAU 246 meeting in Capri, Italy, glossing over the well-known results from the literature, but paying particular attention to new, previously unpublished material. This new material includes a careful comparison of the apparently contradictory results of two independent methods used to simulate the evolution of binary populations in dense stellar systems (the direct N-body method of Hurley, et al. 2007 and the approximate Monte Carlo method of Ivanova, et al. 2005), that shows that the two methods may not actually yield contradictory results, and suggests future work to more directly compare the two methods.
7 pages, 1 figure, to appear in "Dynamical Evolution of Dense Stellar Systems", IAUS 246, ed. E. Vesperini
References in corpus (5)
- The core binary fractions of star clusters from realistic simulations
- Ratios of star cluster core and half-mass radii: a cautionary note on intermediate-mass black holes in star clusters
- The effect of stellar-mass black holes on the structural evolution of massive star clusters
- Star Clusters with Primordial Binaries: III. Dynamical Interaction between Binaries and an Intermediate Mass Black Hole
- Dynamical evidence for intermediate mass black holes in old globular clusters