Differentially rotating neutron stars with dark matter cores

TL;DR

This paper models neutron stars with dark matter cores, analyzing how dark matter influences their structure and rotation, which is vital for understanding their stability and evolution post-merger.

Contribution

It extends numerical modeling to include dark matter as a self-interacting bosonic condensate in differentially rotating neutron stars, a novel approach.

Findings

Constructed equilibrium sequences for dark matter neutron stars.

Analyzed the impact of dark matter on rotational dynamics.

Provided a framework for future studies of dark matter effects.

Abstract

Dark matter is expected to accumulate inside neutron stars, modifying the structure of isolated stars and influencing both the dynamics of binary mergers and the evolution of the resulting hypermassive remnants. Since differential rotation is the primary mechanism delaying the collapse of these remnants, understanding its behavior is crucial when assessing the impact of an embedded dark component. In this work, we extend the numerical code RNS to describe two gravitationally coupled fluids in differential rotation, with baryonic matter modeled by a realistic nuclear equation of state and dark matter represented as a self-interacting bosonic condensate. Within this framework, we construct equilibrium sequences for a representative differential rotation law, providing a basis to explore how dark matter may influence the global properties and rotational dynamics of binary neutron star remnants.