Gravothermal Evolution of Dark Matter Halos: Insights from Self-Interacting and Dissipative Models

Abstract

Gravothermal simulations provide an idealized framework to study the thermal evolution of self-gravitating systems, treating halos as spherically symmetric, pressure-supported structures evolving under the effects of energy transport. These simulations have been widely used to model self-interacting dark matter (SIDM) halos, where heat conduction redistributes energy, leading to core formation and eventual collapse. In dissipative dark matter models, where interactions involve energy loss, this collapse can occur on much shorter timescales. This work focuses on implementing and validating a gravothermal simulation framework for studying the evolution of SIDM and dissipative halos. By numerically solving the coupled equations of mass conservation, hydrostatic equilibrium, and energy transport, we investigate the dependence of collapse timescales on initial halo profiles. Specifically, we compare the evolution of halos initialized with Navarro-Frenk-White (NFW) and DK14 density profiles to demonstrate how differences in initial conditions affect the onset and progression of core collapse. Rather than presenting new physical insights, this study aims to systematically establish a framework for reproducing and analyzing gravothermal evolution under different assumptions. The results reinforce the role of initial density structure in determining the collapse behavior of dark matter halos, providing a basis for future extensions incorporating additional physical effects.