Maximally self-interacting dark matter: models and predictions

Abstract

We study self-interacting dark matter (SIDM) scenarios, where the s-wave selfscattering cross section almost saturates the Unitarity bound. Such self-scattering cross sections are featured by strong velocity dependence in a wide range of velocities. They may be indicated by observations of dark matter halos in a wide range of masses, from Milky Way's dwarf spheroidal galaxies to galaxy clusters. We pin down the model parameters that saturates the Unitarity bound in well-motivated SIDM models: the gauged L µ − L τ model and composite asymmetric dark matter model. We discuss implications and predictions of such model parameters for cosmology like the H 0 tension and dark-matter direct-detection experiments, and particle phenomenology like the beam-dump experiments.

Self-interacting Inelastic Dark Matter in the light of XENON1T excess

“…5 as measured from astrophysical data. The data includes measurements from dwarfs (red), LSBs (blue) and clusters (green) [17,69]. The purple dashed curve corresponds to the velocity-dependent cross section from our model for a particular set of benchmark values (i.e M ψ = 1 GeV, M Z = 50 MeV and α = 0.001) allowed from all relevant phenomenological constraints.…”

Late-Time Dark Matter Oscillations and the Core-Cusp Problem

“…Like other exothermic processes, this has the advantage of predicting a cross section with σv remaining constant at low velocities, as desired for fitting the DM profiles of both large and small galactic structures. Other interesting possibilities to achieve the correct velocity-dependence of SIDM have been studied, for instance in the context of resonant SIDM [9][10][11], puffy DM [12], self-heating DM [13], maximally SIDM [14] and DM bound states produced in the early universe by threebody recombination [15,16].…”

The Role of Non-Governmental Organizations in Protection and Promotion of Child Rights in the North Lakhimpur Sub-Division of Lakhimpur District of Assam

“…We also plot the self-scattering cross-section per unit DM mass as a function of average collision velocity, which fits the available data from dwarfs (red), low surface brightness (LSB) galaxies (blue), and clusters (green) [17,71]…”