An Extended Parametric Model for Self-interacting Dark Matter Halos

TL;DR

This paper enhances a parametric model for SIDM halo evolution by incorporating mass accretion effects, leading to more accurate predictions of halo properties like $V_{max}$.

Contribution

The authors extend the existing SIDM halo evolution model to include mass accretion effects, improving its accuracy against cosmological simulations.

Findings

The extended model reduces errors in $V_{max}$ predictions.

Mass accretion delays core-collapse in SIDM halos.

The model aligns better with cosmological simulation results.

Abstract

We improve upon the parametric model for the evolution of the density profiles of self-interacting dark matter (SIDM) halos introduced in Yang et al. (2024b), by considering the effects of mass accretion on a SIDM halo's gravothermal evolution. The original parametric model accurately predicts parameters $V_{\max}$ and $R_{\max}$, but with a tendency to overpredict $V_{\max}$ at $z=0$ for a subset of field halos. This discrepancy results from the parametric model predicting a faster rate of gravothermal evolution for these field halos compared to that measured in cosmological zoom-in simulations. We propose that the effects of mass accretion on the evolution of SIDM halos are not fully captured by the original parametric model. Our extended parametric model assumes that smooth mass accretion delays core-collapse by driving the SIDM halo back toward a Navarro-Frenk-White (NFW) profile (as it would have in the case of cold dark matter). We find that this extended model is able to substantially reduce the error in predicted $V_{\max}$ for halos compared to the original model, providing a more accurate model of SIDM halo evolution.