Self-interacting inelastic dark matter: A viable solution to the small scale structure problems

TL;DR

This paper explores inelastic self-interacting dark matter models with light mediators, demonstrating they can address small-scale structure issues while satisfying observational constraints through velocity-dependent interactions and kinematic suppression.

Contribution

It provides an exact numerical analysis of inelastic dark matter interactions, identifying parameter regions that solve small-scale problems and evade detection constraints.

Findings

Identifies parameter space where self-interacting dark matter resolves small-scale issues.

Shows inelastic interactions can suppress direct detection signals.

Demonstrates compatibility with relic abundance and observational constraints.

Abstract

Self-interacting dark matter has been proposed as a solution to the small-scale structure problems, such as the observed flat cores in dwarf and low surface brightness galaxies. If scattering takes place through light mediators, the scattering cross section relevant to solve these problems may fall into the non-perturbative regime leading to a non-trivial velocity dependence, which allows compatibility with limits stemming from cluster-size objects. However, these models are strongly constrained by different observations, in particular from the requirements that the decay of the light mediator is sufficiently rapid (before Big Bang Nucleosynthesis) and from direct detection. A natural solution to reconcile both requirements are inelastic endothermic interactions, such that scatterings in direct detection experiments are suppressed or even kinematically forbidden if the mass splitting between the two-states is sufficiently large. Using an exact solution when numerically solving the Schr\"odinger equation, we study such scenarios and find regions in the parameter space of dark matter and mediator masses, and the mass splitting of the states, where the small scale structure problems can be solved, the dark matter has the correct relic abundance and direct detection limits can be evaded.