AHWK - MCLUSTER

AHWK	RESEARCH DOWNLOADS LINKS
Andreas H.W. Küpper Department of Astronomy Yale University 260 Whitney Avenue New Haven, CT 06511 ahwkuepper(at)gmail.com
	McLuster - a Tool to make a Star Cluster Files McLuster source code [build 1 April 2013] 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 Send a mail to ahwkuepper(at)gmail.com 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) NEW! Nuker (Lauer et al. 1995) 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 determine half-mass radius according to Marks & Kroupa (2012) 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 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 Kroupa (2001) IMF with optimal sampling (Kroupa et al. 2011) L3 IMF (Maschberger 2012) 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 NEW! determined using the Sana & Evans (2011) period distribution (for high-mass binaries) apply Kroupa (1995) eigenevolution to short-period binaries NEW! use Sana & Evans (2011) eccentricity distribution for high-mass binaries evolve binaries using BSE (Hurley, Tout & Pols 2002) OpenMP multi-core usage for high performance