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=1.5× 106 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 ˜ 2 times faster than that predicted by the generalized Chandrasekhar formula; ii) the progenitor clusters merge in less than 20 galactic core-crossing time (t_b); iii) the NC configuration keeps a quasi-stable state at least within ˜ 70 t_b.
Simulations of nuclear cluster formation / Miocchi, Paolo; CAPUZZO DOLCETTA, Roberto Angelo. - In: MEMORIE DELLA SOCIETÀ ASTRONOMICA ITALIANA. - ISSN 0037-8720. - ELETTRONICO. - 80:(2009), pp. 50-51. (Intervento presentato al convegno LII Convegno Nazionale della Società Astronomica Italiana tenutosi a Teramo (Italy) nel 4-8 May 2009).
Simulations of nuclear cluster formation .
MIOCCHI, PAOLO;CAPUZZO DOLCETTA, Roberto Angelo
2009
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=1.5× 106 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 ˜ 2 times faster than that predicted by the generalized Chandrasekhar formula; ii) the progenitor clusters merge in less than 20 galactic core-crossing time (t_b); iii) the NC configuration keeps a quasi-stable state at least within ˜ 70 t_b.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
