Multimass spherical structure models for N-body simulations

Details Multimass spherical structure models for N-body simulations Multimass spherical structure models for N-body simulations

2007-10-16

arxiv.org/abs/0710.3189v2

Monthly Notices of the Royal Astronomical Society, Volume 386, Issue 3, Pages 1543-1556, 2008

Astronomy and Astrophysics

Astrophysics

13 pages, 8 figures, 3 tables, replaced version that matches published version

Scientific paper

10.1111/j.1365-2966.2008.13126.x

We present a simple and efficient method to set up spherical structure models for N-body simulations with a multimass technique. This technique reduces by a substantial factor the computer run time needed in order to resolve a given scale as compared to single-mass models. It therefore allows to resolve smaller scales in N-body simulations for a given computer run time. Here, we present several models with an effective resolution of up to 1.68 x 10^9 particles within their virial radius which are stable over cosmologically relevant time-scales. As an application, we confirm the theoretical prediction by Dehnen (2005) that in mergers of collisonless structures like dark matter haloes always the cusp of the steepest progenitor is preserved. We model each merger progenitor with an effective number of particles of approximately 10^8 particles. We also find that in a core-core merger the central density approximately doubles whereas in the cusp-cusp case the central density only increases by approximately 50%. This may suggest that the central region of flat structures are better protected and get less energy input through the merger process.

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