Primordial magnetic fields via spontaneous breaking of Lorentz invariance

Bertolami, Orfeu; Mota, David F.

doi:10.1016/s0370-2693(99)00418-9

Cited by 132 publications

(113 citation statements)

References 33 publications

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“…Therefore, the effective mass for the massive vector particle composing the cosmological gas filling the Universe, and representing its main matter component, may have originated during inflation [18]. The mass of the cosmological vector particle can also be acquired from the spontaneous breaking of Lorentz symmetry in the context of field theories arising from string field theory, or due to the introduction of a fundamental minimal length in a trans-Planckian physics scenario [19].…”

Section: Discussion and Final Remarksmentioning

confidence: 99%

Dark energy as a massive vector field

2007

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We propose that the Universe is filled with a massive vector field, non-minimally coupled to gravitation. The field equations of the model are consistently derived and their application to cosmology is considered. The Friedmann equations acquire an extra dark-energy component, which is proportional to the mass of the vector particle. This leads to a late-time accelerated de Sitter type expansion. The free parameters of the model (gravitational coupling constants and initial value of the cosmological vector field) can be estimated by using the PPN solar system constraints.The mass of the cosmological massive vector particle, which may represent the main component of the Universe, is of the order of 10 −63 g.

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Section: Discussion and Final Remarksmentioning

confidence: 99%

Dark energy as a massive vector field

2007

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“…with q = 3(3 + p)/(4 p), and where κ 18 , κ 19 , κ 20 , κ 21 are given in Appendix A. In the above equations, we have assumed that…”

Section: Evolution Laws In a Radiation-dominated Universementioning

confidence: 99%

Evolution of primordial magnetic fields in mean-field approximation

Campanelli

2014

Eur. Phys. J. C

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We study the evolution of phase-transitiongenerated cosmic magnetic fields coupled to the primeval cosmic plasma in the turbulent and viscous free-streaming regimes. The evolution laws for the magnetic energy density and the correlation length, both in the helical and the non-helical cases, are found by solving the autoinduction and Navier-Stokes equations in the mean-field approximation. Analytical results are derived in Minkowski spacetime and then extended to the case of a Friedmann universe with zero spatial curvature, both in the radiation-and the matterdominated era. The three possible viscous free-streaming phases are characterized by a drag term in the Navier-Stokes equation which depends on the free-streaming properties of neutrinos, photons, or hydrogen atoms, respectively. In the case of non-helical magnetic fields, the magnetic intensity B and the magnetic correlation length ξ B evolve asymptotically with the temperature, T , asHere, T i , N i , and v i are, respectively, the temperature, the number of magnetic domains per horizon length, and the bulk velocity at the onset of the particular regime. The coefficients κ B , κ ξ , 1 , 2 , 3 , and 4 , depend on the index of the assumed initial power-law magnetic spectrum, p, and on the particular regime, with the order-one constants κ B and κ ξ depending also on the cutoff adopted for the initial magnetic spectrum. In the helical case, the quasi-conservation of the magnetic helicity implies, apart from logarithmic corrections and a factor proportional to the initial fractional helicity, power-like evolution laws equal to those in the non-helical case, but with p equal to zero.

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“…In that case, if galactic magnetism is of cosmological origin it may carry information as regards QG physics, since the inflationary era, where quantum fluctuations are generated, is some orders of magnitude close to the Planck scale. In fact, there are several studies on the connection between LV and the survival of cosmological magnetic fields [50][51][52][53][54][55][56]. The basic framework to build a realistic effective field theory for LV in curved space-time is the standard-model-extension (SME) [57,58], where particles follow Finslerian geodesics [59][60][61].…”

Section: Introductionmentioning

confidence: 99%

Cosmic magnetization in curved and Lorentz violating space–times

Kouretsis

2014

Eur. Phys. J. C

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The presence of the large-scale magnetic fields is one of the greatest puzzles of contemporary cosmology. The symmetries of the electromagnetic field theory combined with the geometric structure of the FRW universe leads to an adiabatic decay of the primordial magnetic fields. Due to this rapid decay the residual large-scale magnetic field is astrophysically unimportant. A common feature among many of the proposed amplification mechanisms is the violation of Lorentz symmetries. We introduce an amplification mechanism within a Lorentz violating environment where we use Finsler geometry as our theoretical background. The mechanism is based on the adoption of a local anisotropic structure that leads to modifications on the Ricci identities. Thus, the wave-like equation of any vector source, including the magnetic field, is enriched by the Finslerian curvature theory. In particular limits, the remaining seed field can be strong enough to seed the galactic dynamo. In our analysis we also develop the 1+3 covariant formalism for the 4-vector potential in curved space-times.

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Primordial magnetic fields via spontaneous breaking of Lorentz invariance

Cited by 132 publications

References 33 publications

Dark energy as a massive vector field

Dark energy as a massive vector field

Evolution of primordial magnetic fields in mean-field approximation

Cosmic magnetization in curved and Lorentz violating space–times

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