The velocity anisotropy - density slope relation

Abstract

One can solve the Jeans equation analytically for equilibrated dark matter structures, once given two pieces of input from numerical simulations. These inputs are 1) a connection between phase-space density and radius, and 2) a connection between velocity anisotropy and density slope, the α-βrelation. The first (phase-space density v.s. radius) has already been analysed through several different simulations, however the second (α-βrelation) has not been quantified yet. We perform a large set of numerical experiments in order to quantify the slope and zero-point of the α-βrelation. We find strong indication that the relation is indeed an attractor. When combined with the assumption of phase-space being a power-law in radius, this allows us to conclude that equilibrated dark matter structures indeed have zero central velocity anisotropy β_0 = 0, central density slope of α_0 = -0.8, and outer anisotropy of β_\infty = 0.5.

15 pages, 7 figures

References in corpus (6)

• Convergence and scatter of cluster density profiles
• A universal density slope - velocity anisotropy relation for relaxed structures
• Dark matter distribution function from non-extensive statistical mechanics
• Dark matter density profiles from the Jeans equation
• Circular velocity profiles of dark matter haloes
• Scale Radii and Aggregation Histories of Dark Haloes

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• Dark Matter Direct Search Rates in Simulations of the Milky Way and Sagittarius Stream
• The nature of dark matter and the density profile and central behavior of relaxed halos
• Large-Scale Velocity Dispersion and the Cosmic Web
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• Power law pseudo phase-space density profiles of dark matter halos: fluke of physics?
• Estimating the dark matter velocity anisotropy to the cluster edge
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