Magnetic fields appear at all scales in the Universe, spanning many orders of magnitude in their strength, and intervening in the development of many astrophysical processes. In particular, in compact objects, magnetic fields can reach huge intensities and play a fundamental role in the evolution of the star and its surroundings. In this review, the most relevant ideas about their generation mechanisms and their eects on the composition and evolution of compact stars are summarized. The review highlights the role played by anisotropic pressures, induced by the presence of strong magnetic fields, in the equation of state and in the macroscopic observables of compact objects. Anisotropies demand to solve Einstein equations beyond the sphericalsymmetry. In this regard, two models are analyzed, one using a metric in cylindrical coordinates and another one considering a metric, which allows to take into account small deformations of the objects. These results are relevant for the description of magnetized white dwarfs and hypothetical quark and Bose-Einstein condensate stars. Some related astrophysical phenomena, as pulsar kick velocities and jets associated to compact objects, are also addressed as a consequence of the presence of strong magnetic fields.
An outlook of different aspects of the incidence of magnetic fields on early universe events is presented. The events we will focus on include inflation and the electroweak phase transition. The guideline of the study is mainly the effect of the magnetic field on the effective potential of phase transitions and the decay process of the field leading the phase transition. We will consider both weak and strong magnetic field approximations, since this issue seems to make some important differences in the results. Besides presenting the results of our working group, we will also discuss other works that can be found in the literature.
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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