The impact of inelastic self-interacting dark matter on the dark matter structure of a Milky Way halo

TL;DR

This study investigates how inelastic self-interacting dark matter alters the internal structure and velocity distribution of a Milky Way-sized halo, revealing potential observable signatures for dark matter detection.

Contribution

It introduces a novel inelastic two-state dark matter model into simulations, demonstrating its effects on halo density, shape, and particle velocities compared to elastic SIDM and CDM.

Findings

Inelastic SIDM reduces central halo density faster than elastic SIDM.

Inelastic collisions produce high-velocity unbound particles up to 500 km/s.

Inelastic SIDM results in a more spherical inner halo than CDM.

Abstract

We study the effects of inelastic dark matter self-interactions on the internal structure of a simulated Milky Way (MW)-size halo. Self-interacting dark matter (SIDM) is an alternative to collisionless cold dark matter (CDM) which offers a unique solution to the problems encountered with CDM on sub-galactic scales. Although previous SIDM simulations have mainly considered elastic collisions, theoretical considerations motivate the existence of multi-state dark matter where transitions from the excited to the ground state are exothermic. In this work, we consider a self-interacting, two-state dark matter model with inelastic collisions, implemented in the Arepo code. We find that energy injection from inelastic self-interactions reduces the central density of the MW halo in a shorter timescale relative to the elastic scale, resulting in a larger core size. Inelastic collisions also isotropize the orbits, resulting in an overall lower velocity anisotropy for the inelastic MW halo. In the inner halo, the inelastic SIDM case (minor-to-major axis ratio $s \equiv c/a \approx 0.65$) is more spherical than the CDM ($s \approx 0.4$), but less spherical than the elastic SIDM case ($s \approx 0.75$). The speed distribution $f(v)$ of dark matter particles at the location of the Sun in the inelastic SIDM model shows a significant departure from the CDM model, with $f(v)$ falling more steeply at high speeds. In addition, the velocity kicks imparted during inelastic collisions produce unbound high-speed particles with velocities up to 500 km s$^{-1}$ throughout the halo. This implies that inelastic SIDM can potentially leave distinct signatures in direct detection experiments, relative to elastic SIDM and CDM.