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Anomalous X-ray Pulsars (AXPs) and Soft Gamma-Ray Repeaters (SGRs) are youngneutron stars (NSs) characterized by high X-ray quiescent luminosities,outbursts, and, in the case of SGRs, sporadic giant flares. They are believedto be powered by ultra-strong magnetic fields (hence dubbed magnetars). Thediversity of their observed behaviours is however not understood, and made evenmore puzzling by the discovery of magnetar-like bursts from "low-field"pulsars. Here we perform long-term 2D simulations that follow the evolution ofmagnetic stresses in the crust; these, together with recent calculations of thebreaking stress of the neutron star crust, allow us to establish whenstarquakes occur. For the first time, we provide a quantitative estimate of theburst energetics, event rate, and location on the neutron star surface, whichbear a direct relevance for the interpretation of the overall magnetarphenomenology. 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 fundamentalseparation among what constitutes the apparent different classes. Among the keyelements that create the variety of observed phenomena, age is more importantthan a small variation in magnetic field strength. We find that outbursts canalso be produced in old, lower-field pulsars (B ~ a few x 10^{12} G), but thoseevents are much less frequent than in young, high-field magnetars.

A unified model of the magnetar and radio pulsar bursting phenomenology