A unified model of the magnetar and radio pulsar bursting phenomenology

TL;DR

This paper presents a comprehensive model explaining the diverse bursting behaviors of magnetars and radio pulsars through long-term simulations of crustal magnetic stress evolution and starquake energetics.

Contribution

It introduces a quantitative framework linking magnetic stress buildup to burst occurrence, unifying magnetar and pulsar phenomena without strict class boundaries.

Findings

Magnetic stress accumulation leads to starquakes and bursts.

Outburst activity correlates more with age than magnetic field strength.

Old, low-field pulsars can produce bursts, but less frequently.

Abstract

Anomalous X-ray Pulsars (AXPs) and Soft Gamma-Ray Repeaters (SGRs) are young neutron stars (NSs) characterized by high X-ray quiescent luminosities, outbursts, and, in the case of SGRs, sporadic giant flares. They are believed to be powered by ultra-strong magnetic fields (hence dubbed magnetars). The diversity of their observed behaviours is however not understood, and made even more puzzling by the discovery of magnetar-like bursts from "low-field" pulsars. Here we perform long-term 2D simulations that follow the evolution of magnetic stresses in the crust; these, together with recent calculations of the breaking stress of the neutron star crust, allow us to establish when starquakes occur. For the first time, we provide a quantitative estimate of the burst energetics, event rate, and location on the neutron star surface, which bear a direct relevance for the interpretation of the overall magnetar phenomenology. Typically, an "SGR-like" object tends to be more active than an "AXP-like" object or a "high-$B$ radio pulsar", but there is no fundamental separation among what constitutes the apparent different classes. Among the key elements that create the variety of observed phenomena, age is more important than a small variation in magnetic field strength. We find that outbursts can also be produced in old, lower-field pulsars (B ~ a few x 10^{12} G), but those events are much less frequent than in young, high-field magnetars.