Abstract
The differential rotation of plasma in the core of pulsars (Ωs ≠ Ωe) generates convective currents increasing with time which in turn generates the toroidal magnetic field. To avoid difficulties of physical interpretation inherent to the theory of general relativity we have adopted the tetrad approach to discuss the generation of the magnetic field in the core of the neutron stars. The results which we have obtained are in agreement with those obtained earlier.
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Published in Astrofizika, Vol. 49, No. 4, pp. 613–620 (August 2006).
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Sedrakian, D.M., Krikorian, R. Toroidal magnetic field in pulsars. Astrophysics 49, 523–529 (2006). https://doi.org/10.1007/s10511-006-0050-y
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DOI: https://doi.org/10.1007/s10511-006-0050-y