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Hall drift of axisymmetric magnetic fields in solid neutron star matter

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Figure

Fig. 1. A meridional cut of a spherical star with an assumed electron density profile n(r) = n 0 [1 − (r/r 0 ) 2 ], where r is the (spherical) radial coordinate, r 0 is the stellar radius, and n 0 is the electron density at r = 0.
Fig. 2. The evolution of a weak poloidal magnetic field component af- af-fected by a much stronger toroidal background field

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