The Angular Momenta of Neutron Stars and Black Holes as a Window on Supernovae

TL;DR

This paper investigates the angular momentum of neutron stars and black holes to understand supernova mechanisms, finding distinct distributions that support different explosion models and jet formation scenarios.

Contribution

It provides the first comparative analysis of angular momentum distributions of neutron stars and black holes, linking them to supernova types and jet production.

Findings

Black holes generally have higher angular momentum than neutron stars.

Distributions suggest black holes originate from jet-producing supernovae.

Neutron stars may be born with high spin but spin down rapidly.

Abstract

It is now clear that a subset of supernovae display evidence for jets and are observed as gamma-ray bursts. The angular momentum distribution of massive stellar endpoints provides a rare means of constraining the nature of the central engine in core-collapse explosions. Unlike supermassive black holes, the spin of stellar-mass black holes in X-ray binary systems is little affected by accretion, and accurately reflects the spin set at birth. A modest number of stellar-mass black hole angular momenta have now been measured using two independent X-ray spectroscopic techniques. In contrast, rotation-powered pulsars spin-down over time, via magnetic braking, but a modest number of natal spin periods have now been estimated. For both canonical and extreme neutron star parameters, statistical tests strongly suggest that the angular momentum distributions of black holes and neutron stars are markedly different. Within the context of prevalent models for core-collapse supernovae, the angular momentum distributions are consistent with black holes typically being produced in GRB-like supernovae with jets, and with neutron stars typically being produced in supernovae with too little angular momentum to produce jets via magnetohydrodynamic processes. It is possible that neutron stars are imbued with high spin initially, and rapidly spun-down shortly after the supernova event, but the available mechanisms may be inconsistent with some observed pulsar properties.