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Bearing in mind the application to the outer crust of the neutron stars(NSs), we investigate the magnetic field decay by means of the fullyrelativistic Particle-In-Cell simulations. Numerical computations are carriedout in 2-dimensions, in which the initial magnetic fields are set to becomposed both of the uniform magnetic fields that model the global fieldspenetrating the NS and of the turbulent magnetic fields that would beoriginated from the Hall cascade of the large-scale turbulence. Our resultsshow that the whistler cascade of the turbulence transports the magnetic energypreferentially in the direction perpendicular to the uniform magnetic fields.It is also found that the distribution function of electrons becomesanisotropic because electrons with lower energies are predominantly heated inthe direction parallel to the uniform magnetic fields due to the Landauresonance, while electrons with higher energies are heated mainly by thecyclotron resonance that makes the distribution function isotropic for the highenergy tails. Furthermore we point out that the degree of anisotropy takesmaximum as a function of the initial turbulent magnetic energy. As analternative to the conventional ohmic dissipation, we propose that the magneticfields in the outer crust of NSs, cascading down to the electron inertial scalevia the whistler turbulence, would decay predominantly by the dissipationprocesses through the Landau damping and the cyclotron resonance.

Magnetic Field Decay Due to the Wave-Particle Resonances in the Outer Crust of the Neutron Star