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Magnetic field evolution in magnetar crusts through three dimensional simulations

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Figure

Figure 1. Magnetic field lines in the simulation with an initially ditially twisted magnetic field consisting of ananfferen- ℓ = 1 (dipole) poloidal and ℓ = 2 toroidal field, starting with only 10−4 of the magnetic energy inthe non-axisymmetric field, (run QU05
Figure 2. Contour plot of the radial (left), latitudinal (middle) and azimuthal (right) component of the magnetic field at r = 0.995R∗ at t = 0 (top) and t = 15kyr(bottom) for the simulation shown in Figure 1.
Figure 3. The maximum magnetic field strength (dashed line) at the surfaceof the star versus the dipole field in three simulations
Figure 4. The Ohmic heating rate versus time for the same simulations asimuthal components decrease monotonically in the crust and the field re-mains mostly axisymmetric; and a simulation where the structure of thefield is identical to that of the blue line,

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