The asymptotic tidal remnants of cold dark matter subhalos

TL;DR

This study uses N-body simulations to analyze how cold dark matter subhalos evolve under tidal forces, revealing how their density profiles and survival depend on orbital parameters and resolution, with implications for Milky Way satellite predictions.

Contribution

It provides a detailed empirical model of tidal remnant evolution, highlighting the importance of resolution and orbital dynamics in subhalo survival and structure.

Findings

Tidal remnants' density profiles depend on mass loss fraction.

High-resolution simulations are crucial for accurate subhalo modeling.

Most subhalos are heavily stripped after ~10 Gyrs, affecting satellite predictions.

Abstract

We use N-body simulations to study the evolution of cuspy cold dark matter (CDM) halos in the gravitational potential of a massive host. Tidal mass losses reshape CDM halos, leaving behind bound remnants whose characteristic densities are set by the mean density of the host at the pericentre of their respective orbit. The evolution to the final bound remnant state is essentially complete after ~5 orbits for nearly circular orbits, while reaching the same remnant requires ~25 and ~40 orbits for eccentric orbits with 1:5 and 1:20 pericentre-to-apocentre ratios, respectively. The density profile of tidal remnants is fully specified by the fraction of mass lost, and approaches an exponentially-truncated Navarro-Frenk-White profile in the case of heavy mass loss. Resolving tidal remnants requires excellent numerical resolution; poorly resolved subhalos have systematically lower characteristic densities and are more easily disrupted. Even simulations with excellent spatial and time resolution fail when the final remnant is resolved with fewer than 3000 particles. We derive a simple empirical model that describes the evolution of the mass and the density profile of the tidal remnant applicable to a wide range of orbital eccentricities and pericentric distances. Applied to the Milky Way, our results suggest that $10^8$ - $10^{10}$ solar mass halos accreted ~10 Gyrs ago on 1:10 orbits with pericentric distance ~10 kpc should have been stripped to 0.1 - 1 per cent of their original mass. This implies that estimates of the survival and structure of such halos (the possible hosts of ultra-faint Milky Way satellites) based on direct cosmological simulations may be subject to substantial revision.