Binary systems, star clusters and the Galactic-field population. Applied stellar dynamics

Details Binary systems, star clusters and the Galactic-field population. Applied stellar dynamics Binary systems, star clusters and the Galactic-field population. Applied stellar dynamics

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mst...........k&link_type=abstract

Habilitation Thesis, Mathematisch-Naturwissenschaftlichen Fakultät der Christian-Albrechts Universität Kiel, Germany. XV + 232 p

Mathematics

4

Binary Systems, Star Clusters, Galaxy, Stellar Dynamics

Scientific paper

This book contains the results of recent theoretical work on the evolution of primordial binary systems in young star clusters, their effect on the evolution of their host clusters, implications for the distribution of young stars in the Milky Way, and the formation of bound star clusters. This work shows that if the Galactic-field binary population is a dynamically evolved version of the Taurus-Auriga pre-main sequence population, then most stars form in clusters with typically a few hundred binaries within a radius of about 0.5-1 pc. The results also suggest that the population I primordial binary-star orbital-parameter distribution functions may be universal, much like the initial mass function. Most solar-like planetary systems can survive in such clusters. The work presented here also establishes that most observed triple and quadruple systems must be primordial, but that α Cen A/B-Proxima Cen-like systems can form in clusters through dynamical capture. Precise N-body calculations using Aarseth's N-body codes of clusters containing up to 104 stars are used to create an extensive young-cluster library. These data demonstrate that the primordial binary systems are disrupted on a crossing-time scale, and that the truncation of the surviving period distribution measures the maximum concentration the cluster ever experienced. The N-body calculations demonstrate that Galactic star clusters form readily as nuclei of expanding OB associations despite a star-formation efficiency of typically 30 per cent and gas-expulsion over a time-span shorter than the cluster crossing time.

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