Simulations of Nuclear Cluster formation
Abstract
Preliminary results are presented about a fully self-consistent N-body simulation of a sample of four massive globular clusters in close interaction within the central region of a galaxy. The N-body representation (with N=1.5x10^6 particles in total) of both the clusters and the galaxy allows to include in a natural and self-consistent way dynamical friction and tidal interactions. The results confirm the decay and merging of globulars as a viable scenario for the formation/accretion of compact nuclear clusters. Specifically: i) the frictional orbital decay is about 2 times faster than that predicted by the generalized Chandrasekhar formula; ii) the progenitor clusters merge in less than 20 galactic core-crossing time; iii) the NC configuration keeps a quasi-stable state at least within 70 galactic core-crossing times.
Cite
@article{arxiv.0902.0472,
title = {Simulations of Nuclear Cluster formation},
author = {P. Miocchi and R. Capuzzo-Dolcetta},
journal= {arXiv preprint arXiv:0902.0472},
year = {2009}
}
Comments
Talk presented at the 52 Congress of the Societa' Astronomica Italiana, held in Teramo (Italy), may 4-8, 2008. Two pages including 2 figures