A non-perturbative study of the evolution of cosmic magnetised sources

Abstract

We undertake a hydrodynamical study of a mixture of tightly coupled primordial radiation, neutrinos, baryons, electrons and positrons, together with a gas of already decoupled dark matter WIMPS and an already existing "frozen" magnetic field in the infinite conductivity regime. Considering this cosmic fluid as the source of a homogeneous but anisotropic Bianchi I model, we describe its interaction with the magnetic field by means of suitable equations of state that are appropriate for the particle species of the mixture between the end of the leptonic era and the beginning of the radiation-dominated epoch. Fulfilment of observational bounds on the magnetic field intensity yields a "near FLRW" (but strictly non-perturbative) evolution of the geometric, kinematic and thermodynamical variables. This evolution is roughly comparable to the weak field approximation in linear perturbations on a spatially flat FLRW background of sources in which the frozen magnetic fields are coherent over very large supra-horizon scales. Our approach and results may provide interesting guidelines in potential situations in which non-perturbative methods are required to study the interaction between magnetic fields and the cosmic fluid.

Kicks of magnetized strange quark stars induced by anisotropic emission of neutrinos

“…Effects on the structure equations come from this anisotropy in the energy-momentum tensor. In previous works, the anisotropic effect of magnetic fields on the EoS for white dwarfs (WD), neutron stars and quark stars (QS) [10][11][12] as well as for the evolution of the early universe [13] have been studied. The possibility that unpaired magnetized quark matter be in a superconductor state, and in particular in the CFL phase, was explored in Refs.…”