Formation and Evolution of the Self-Interacting Dark Matter Halos

  title={Formation and Evolution of the Self-Interacting Dark Matter Halos},
  author={Kyungjin Ahn and Paul R. Shapiro},
  journal={arXiv: Astrophysics},
We have derived the first, fully-cosmological, similarity solutions for CDM halo formation in the presence of nongravitational collisionality, which provides an analytical theory of the effect of the self-interacting dark matter (SIDM) hypothesis on halo density profiles. Collisions transport heat inward, which produces a constant-density core, while continuous infall pumps energy into the halo to stabilize the core against gravothermal catastrophe. These solutions improve upon earlier attempts… 
Dynamical Instability of Collapsed Dark Matter Halos
  • Wei-Xiang Feng, Hai-Bo Yu, Yi-Ming Zhong
  • Physics
  • 2021
A self-interacting dark matter halo can experience gravothermal collapse, resulting in a central core with an ultrahigh density. It can further contract and collapse into a black hole, a mechanism
Dark matter concentrations in galactic nuclei according to polytropic models
We calculate the radial profiles of galaxies where the nuclear region is self-gravitating, consisting of self-interacting dark matter (SIDM) with F degrees of freedom. For sufficiently high density
Core formation from self-heating dark matter
Cosmological simulations of the $\Lambda$CDM model suggest that the dark matter halos of dwarf galaxies are denser in their center than what observational data of such galaxies imply. In this letter,
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure
We use cosmological simulations to study the effects of self-interacting dark matter (SIDM) on the density profiles and substructure counts of dark matte r halos from the scales of spiral galaxies to
Galaxy stability within a self-interacting dark matter halo
This paper investigates spheroidal galaxies comprising a self-interacting dark matter halo (SIDM) plus de Vaucouleurs stellar distribution. These are coupled only via their shared gravitational
Gravothermal collapse of isolated self-interacting dark matter haloes: N-body simulation versus the fluid model
We make direct comparisons between Monte Carlo N-body simulations and analytic and numerical solutions of a conduction fluid (gaseous) model, for various isolated selfinteracting dark matter (SIDM)
Signatures of self-interacting dark matter on cluster density profile and subhalo distributions
Non-gravitational interactions between dark matter particles with strong scattering, but relatively small annihilation and dissipation, has been proposed to match various observables on cluster and
Dark Matter Self-interactions and Small Scale Structure
We review theories of dark matter (DM) beyond the collisionless paradigm, known as self-interacting dark matter (SIDM), and their observable implications for astrophysical structure in the Universe.
Radial structure, inflow and central mass of stationary radiative galaxy clusters
We analyse the radial structure of self-gravitating spheres consisting of multiple interpenetrating fluids, such as the X-ray emitting gas and the dark halo of a galaxy cluster. In these dipolytropic
Gravitational and distributed heating effects of a cD galaxy on the hydrodynamical structure of its host cluster
We investigate the effects of a cD galaxy’s gravity and AGN heating of the host galaxy cluster. We consider a standard prescription for the hydrodynamics, with the structures determined by mass


We have derived the first, fully cosmological, similarity solutions for cold dark matter (CDM) halo formation in the presence of non-gravitational collisionality (i.e. elastic scattering), which
Self-Interacting Dark Matter Halos and the Gravothermal Catastrophe
We study the evolution of an isolated spherical halo of self-interacting dark matter (SIDM) in the gravothermal fluid formalism. We show that the thermal relaxation time tr of an SIDM halo with the
The Structure and Evolution of Weakly Self-interacting Cold Dark Matter Halos.
  • Burkert
  • Physics, Medicine
    The Astrophysical journal
  • 2000
The evolution of halos consisting of weakly self-interacting dark matter particles is investigated using a new numerical Monte Carlo N-body method, adopting the currently popular LambdaCDM model, and the predicted core radii and core densities are in good agreement with the observations.
Weakly Self-interacting Dark Matter and the Structure of Dark Halos
We study the formation of dark halos in a ΛCDM universe under the assumption that cold dark matter (CDM) particles have a finite cross section for elastic collisions. We compare evolution when CDM
On the Formation and Evolution of Disk Galaxies: Cosmological Initial Conditions and the Gravitational Collapse
We use a semianalytical approach and the standard σ8 = 1 cold dark matter (SCDM) cosmological model to study the gravitational collapse and virialization, the structure, and the global and
Collisional Dark Matter and the Structure of Dark Halos.
The observed rotation curves of dwarf galaxies are argued to argue that self-interacting dark matter can only be viable if intermediate cross sections produce structure that does not lie between the extremes, as in the collisionless case.
Mass growth and density profiles of dark matter haloes in hierarchical clustering
We develop a model for the growth of dark matter haloes and use it to study their evolved density profiles. In this model, haloes are spherical and form by quiescent accretion of matter in clumps,
Formation of Cuspy Density Profiles: A Generic Feature of Collisionless Gravitational Collapse
Using the formalism of the spherical infall model, the structure of collapsed and virialized dark halos is calculated for a variety of scale-free initial conditions. In spite of the scale-free
Dark Halos: The Flattening of the Density Cusp by Dynamical Friction
N-body simulations and analytical calculations of the gravitational collapse in an expanding universe predict that halos should form with a diverging inner density profile, the cusp. There are some
Self-similar Spherical Collapse Revisited: A Comparison between Gas and Dark Matter Dynamics
We reconsider the collapse of cosmic structures in an Einstein-de Sitter universe, using the self-similar initial conditions of Fillmore & Goldreich (1984). We first derive a new approximation to