Magnetar activity mediated by plastic deformations of neutron star crust

TL;DR

This paper proposes a model where magnetar activity results from magnetic field evolution driven by electron MHD flows, crustal plasticity, and magnetospheric reconnection, explaining various observed phenomena including flares and surface emissions.

Contribution

It introduces a 'Solar flare' inspired model linking magnetic field evolution, crustal plastic deformation, and magnetospheric reconnection to magnetar activity.

Findings

Persistent luminosity scales with magnetic field cubed.

Giant flares require magnetic fields above a threshold.

Post-flare surface emission results from whistler pulse dissipation.

Abstract

We advance a "Solar flare" model of magnetar activity, whereas a slow evolution of the magnetic field in the upper crust, driven by electron MHD (EMHD) flows, twists the external magnetic flux tubes, producing persistent emission, bursts and flares. At the same time the neutron star crust plastically relieves the imposed magnetic field stress, limiting the strain $ \epsilon_t $ to values well below the critical strain $ \epsilon_{crit}$ of a brittle fracture, $ \epsilon_t \sim 10^{-2}\epsilon_{crit} $. Magnetar-like behavior, occurring near the magnetic equator, takes place in all neutron stars, but to a different extent. The persistent luminosity is proportional to cubic power of the magnetic field (at a given age), and hence is hardly observable in most rotationally powered neutron stars. Giant flares can occur only if the magnetic field exceeds some threshold value, while smaller bursts and flares may take place in relatively small magnetic fields. Bursts and flares are magnetospheric reconnection events that launch Alfven shocks which convert into high frequency whistlers upon hitting the neutron star surface. The resulting whistler pulse induces a strain that increases with depth both due to the increasing electron density (and the resulting slowing of the waves), and due to the increasing coherence of a whistler pulse with depth. The whistler pulse is dissipated on a time scale of approximately a day at shallow depths corresponding to $\rho \sim 10^{10} {\rm g cm}^{-3}$; this energy is detected as enhanced post-flare surface emission.