Three-dimensional relativistic simulations of rotating neutron-star collapse to a Kerr black hole

TL;DR

This paper introduces a new 3D general-relativistic hydrodynamics code and applies it to simulate the collapse of rotating neutron stars into Kerr black holes, analyzing horizon formation and matter dynamics.

Contribution

The paper presents a novel 3D relativistic simulation code and demonstrates its application to neutron-star collapse, including horizon tracking and matter behavior analysis.

Findings

Black hole mass and spin measured accurately during collapse

No evidence of shocks or stable orbit matter outside black holes

Collapse dynamics strongly depend on initial angular momentum

Abstract

We present a new three-dimensional fully general-relativistic hydrodynamics code using high-resolution shock-capturing techniques and a conformal traceless formulation of the Einstein equations. Besides presenting a thorough set of tests which the code passes with very high accuracy, we discuss its application to the study of the gravitational collapse of uniformly rotating neutron stars to Kerr black holes. The initial stellar models are modelled as relativistic polytropes which are either secularly or dynamically unstable and with angular velocities which range from slow rotation to the mass-shedding limit. We investigate the gravitational collapse by carefully studying not only the dynamics of the matter, but also that of the trapped surfaces, i.e. of both the apparent and event horizons formed during the collapse. The use of these surfaces, together with the dynamical horizon framework, allows for a precise measurement of the black-hole mass and spin. The ability to successfully perform these simulations for sufficiently long times relies on excising a region of the computational domain which includes the singularity and is within the apparent horizon. The dynamics of the collapsing matter is strongly influenced by the initial amount of angular momentum in the progenitor star and, for initial models with sufficiently high angular velocities, the collapse can lead to the formation of an unstable disc in differential rotation. All the simulations performed with uniformly rotating initial data and a polytropic or ideal-fluid equation of state show no evidence of shocks or of the presence of matter on stable orbits outside the black hole.