Abstract
Physical input to the equations which govern the evolution of magnetic fields in non-superconducting parts of neutron star cores is discussed with emphasis to the conductivity of matter. Magnetic fields can be influenced by the effects associated with the balance of forces, by circulation (induced by the heat transport), by anisotropic resistivity of magnetized plasma (Ohmic decay of longitudinal and transverse currents and the Hall drift), etc. The timescales of these processes range from several minutes to the Universe age; the field lifetimes ~ 104 – 107 yr might be expected.
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Yakovlev, D.G. (1991). Electrical Conductivity of Neutron Star Cores and Evolution of Internal Magnetic Fields. In: Ventura, J., Pines, D. (eds) Neutron Stars: Theory and Observation. NATO ASI Series, vol 344. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-3536-8_15
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DOI: https://doi.org/10.1007/978-94-011-3536-8_15
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