The Accretion-Driven Structure and Kinematics of Relaxed Dark Halos

TL;DR

This paper extends the understanding of dark matter halos by deriving their structural and kinematic profiles, including density and velocity dispersion, based on accretion-driven growth models, aligning well with simulation data.

Contribution

It introduces a method to predict detailed profiles of triaxial, anisotropic, rotating halos from accretion-driven growth, expanding previous spherical models.

Findings

Derived density and velocity dispersion profiles match simulation data.

Established relationships between accretion rates and halo structure.

Validated the model against existing N-body simulation results.

Abstract

It has recently been shown that relaxed spherically symmetric dark matter halos develop from the inside out, by permanently adapting their inner structure to the boundary conditions imposed by the current accretion rate. Such a growth allows one to infer the typical density profiles of halos. Here we follow the same approach to infer the typical spherically averaged profiles of the main structural and kinematic properties of triaxial, anisotropic, rotating halos. Specifically, we derive their density, spatial velocity dispersion, phase-space density, anisotropy and specific angular momentum profiles. The results obtained are in agreement with available data on these profiles from \nbody simulations.