We study Faraday rotation in the quantum relativistic limit. Starting from the photon selfenergy in the presence of a constant magnetic field the rotation of the polarization vector of a plane electromagnetic wave which travel along the fermion-antifermion gas is studied. The connection between Faraday Effect and Quantum Hall Effect (QHE) is discussed. The Faraday Effect is also investigated for a massless relativistic (2D+1)-dimensional fermion system which is derived by using the compactification along the dimension parallel to the magnetic field. The Faraday angle shows a quantized behavior as Hall conductivity in two and three dimensions.
The aim of this work is to solve the dispersion relations near the first excitation threshold of a photon propagating along a magnetic field in the strong field limit. We have calculated the time damping of the photon in two particular cases: the degenerate gas as well as the diluted gas limit, both being important from the astrophysical point of view. In particular, the diluted gas limit could describe the magnetosphere of neutron stars. The solutions have been used to obtain a finite quantum Faraday angle in both limits. A resonant behavior for the Faraday angle is also obtained. To reproduce the semi-classical result for the Faraday rotation angle, the weak field limit is considered.
The aim of this work is to study Faraday rotation in the quantum relativistic limit. Starting from the photon self-energy in the presence of a constant magnetic field the rotation of the polarization vector of a plane electromagnetic wave which travels along the fermion-antifermion gas is studied. The connection between Faraday Effect and Quantum Hall Effect (QHE) is discussed. The Faraday angle shows a resonant behavior which is related with the branching points of the Hall conductivity. Possible applications to magnetospheres of compact objects are discussed.
We study the transverse propagation of photons in a magnetized vacuum considering radiative corrections in the one-loop approximation. The dispersion equation is modified due to the magnetized photon self-energy in the transparency region (0 < < 2m e ). The aim of our study is to explore the propagation of photons in a neutron star magnetosphere (described by a magnetized vacuum). The solution of the dispersion equation is obtained in terms of analytic functions. The larger the magnetic field, the higher the phase velocity and the more the dispersion curve deviates from the light-cone. For fixed values of the frequency, we study the dependence of photons time delay with the magnetic field strength, as well as with distance. For the latter, we adopt a magnetic dipole configuration and obtain that, contrary to the expectation, photons of higher energy experience a longer time delay. A discussion of potential causes of this behavior is presented.
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