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Current models of magnetars require extremely strong magnetic fields toexplain their observed quiescent and bursting emission, implying that the fieldstrength within the star's outer crust is orders of magnitude larger than thedipole component inferred from spin-down measurements. This presents a seriouschallenge to theories of magnetic field generation in a proto-neutron star.Here, we present detailed modelling of the evolution of the magnetic field inthe crust of a neutron star through 3-D simulations. We find that, in theplausible scenario of equipartition of energy between global-scale poloidal andtoroidal magnetic components, magnetic instabilities transfer energy tonon-axisymmetric, kilometre-sized magnetic features, in which the local fieldstrength can greatly exceed that of the global-scale field. These intensesmall-scale magnetic features can induce high energy bursts through local crustyielding, and the localised enhancement of Ohmic heating can power the star'spersistent emission. Thus, the observed diversity in magnetar behaviour can beexplained with mixed poloidal-toroidal fields of comparable energies.

Magnetic field evolution in magnetar crusts through three dimensional simulations