Abstract
Using the quantum field theory methods, we calculate the helicity flip of an electron scattering off protons in dense matter of a neutron star. The influence of the electroweak interaction between electrons and background nucleons on the helicity flip is examined. We also derive the kinetic equation for the chiral imbalance. The derived kinetic equation is compared with the results obtained by other authors.
Highlights
Some neutron stars (NS) can possess extremely strong magnetic fields B 1015 G
The detailed computation of the helicity flip rate in ep collisions was the last missing ingredient of the new model, initially proposed in Ref. [2], for the generation of magnetic fields in magnetars driven by the parity violating eN electroweak interaction
The second important result obtained in the present work was the analysis of the influence of the electroweak interaction of colliding electrons with background nucleons on the helicity flip process
Summary
Some neutron stars (NS) can possess extremely strong magnetic fields B 1015 G. These NSs are called magnetars [1]. [2,3,4] we developed the new model for the generation of magnetic fields in magnetars. In this model a large-scale magnetic field in NS can be amplified to the strenth predicted in magnetars owing to the magnetic field instability driven by the electron-nucleon (eN) electroweak interaction. This work is devoted to the further development of the proposed description of the magnetic fields generation in magnetars. We will be interested in the evolution of the chemical potentials of the electron gas in NS in the presence of background nucleons
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