AHWK - MCLUSTER

AHWK	RESEARCH DOWNLOADS LINKS
Andreas H.W. Küpper Argelander-Institut für Astronomie Auf dem Hügel 71 53121 Bonn Raum 3.009, Tel. 73-3653 akuepper(at)astro.uni-bonn.de
	McLuster - a Tool to make a Star Cluster Files McLuster source code [build 13 April 2012] See the README file or the manual for help. Mass segregation and fractal substructure in young massive clusters: (I) the McLuster code and method calibration A.H.W. Küpper, Th. Maschberger, P. Kroupa and H. Baumgardt, 2011, MNRAS, 417, 2300 Please refer to this publication when using McLuster. Mailing List NEW! Send a mail to akuepper(at)astro.uni-bonn.de with "McLuster Mailing List" as subject to receive announcements of critical updates and bug fixes. Features set up clusters for Nbody6, Nbody4 or simply generate a table of stars choose output in Nbody units or in astrophysical units specify either total number of stars or total cluster mass choose one of the following density profiles: Plummer (1911) King (1966) mass-segregated Subr mass-segregated Kroupa & Baumgardt (2007) Elson, Fall & Freeman (1987) homogeneous density specify degree of mass segregation for any profile, from unsegregated to completely segregated specify degree of fractality for any profile, from smooth to completely fractal specify the cluster orbit in one of the following tidal fields: near-field approximation point-mass galaxy full galactic potential consisting of bulge, disk and logarithmic halo NEW! specify an external gas potential for Nbody6 choose stellar mass function between single-mass Kroupa (2001) two-part power-law IMF user-defined multi-power-law IMF NEW! Kroupa (2001) IMF with optimal sampling (Kroupa et al. 2011) set up evolved stellar populations using SSE (Hurley, Pols & Tout 2000) determine maximum stellar mass according to Weidner & Kroupa (2006) relation determine maximum stellar mass for old, evolved populations using the Prantzos (2007) relation specify metallicity either as Z or as [Fe/H] specify either binary fraction or number of binaries choose random pairing or ordered pairing for O and B stars choose between different semi-major axis distributions: flat in a given interval determined using the Kroupa (1995) period distribution determined using the Duquennoy & Mayor (1991) period distribution apply Kroupa (1995) eigenevolution to short-period binaries NEW! evolve binaries using BSE (Hurley, Tout & Pols 2002) NEW! OpenMP multi-core usage for high performance