Electromagnetic field with induced massive term: Case with scalar field

Abstract

Abstract:We consider an interacting system of massless scalar and electromagnetic fields, with the Lagrangian explicitly depending on the electromagnetic potentials, i.e., interaction with broken gauge invariance. The Lagrangian for interaction is chosen in such a way that the electromagnetic field equation acquires an additional term, which in some cases is proportional to the vector potential of the electromagnetic field. This equation can be interpreted as the equation of motion of photon with induced nonzero rest-mass. This system of interacting fields is considered within the scope of Bianchi type-I (BI) cosmological model. It is shown that, as a result of interaction the isotropization process of the expansion takes place. PACS

The Scalar-photon Coupling with Mie Invariant Within the Scope of Bianchi Type-I Cosmological Model

“…We will follow to the algorithm of article [29] taking into account the new action functional (2). Consider anisotropic spatially homogeneous cosmological model of the Bianchi-I type to be described by the metric…”

“…The modern Universe is isotropic, therefore the anisotropic cosmological models must satisfy the criteria isotropization. In article [29] was included the terms (I )∇ ν φ∇ ν φ , where φ is a massless scalar field. It is shown that, as a result of interaction the Bianchi type-I cosmological model is reduced to Friedman's model with the electric field.…”

“…the scalar field induces nonzero rest-mass of photon. In Section 2 our article we extend the model of [29] by introducing additional non-minimal coupling L(I, φ)F μν F μν , where φ is the canonical scalar field or the phantom one. Section 3 presents the case of non-minimal coupling L(I )F μν F μν .…”

Scalar Field in Cosmology: Potential for Isotropization and Inflation

“…It is known as direct problem. Following the second strategy, we invert the problem and construct the effective potential V (ϕ), hence the scalar field ϕ(t) by choosing the appropriate metric function α(t) [37]. This is known as inverse problem.…”

Bianchi type-II cosmological model: some remarks

“…In all other cases one has to write down all the equations. Those equations give relations between the metric functions (if G = 0 and T ≡ 0, as in the case of a Bianchi type-VI space-time with only non-zero diagonal components of the energy-momentum tensor [14]) or material field functions (if G ≡ 0 and T = 0, as in the case of a Bianchi type-I space-time with electro-magnetic fields with A µ = (0 A 1 A 2 A 3 ) [15,16]). Let us now consider the BII cosmological model for a source field with non-zero diagonal components only, i.e., with the energy-momentum tensor given by…”