Seminal magnetic fields from inflato-electromagnetic inflation

Membiela, Federico Agustín; Bellini, Mauricio

doi:10.1140/epjc/s10052-012-2181-0

Cited by 4 publications

(3 citation statements)

References 59 publications

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“…Another approach followed in [52] leads to terms containing scalar fields as well. This differs from an approach of considering five dimensional field with electromagnetic components confined in 1 + 3dimensions [53]. The action for electromagnetic field given by Eq.…”

Section: Magnetogenesis In Gauss-bonnet Gravitymentioning

confidence: 94%

Cosmological magnetogenesis from extra-dimensional Gauss-Bonnet gravity

et al. 2014

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Generation of primordial magnetic fields during inflation typically requires the breaking of conformal invariance of the Electromagnetic action. In this paper this has been achieved naturally in a higher dimensional cosmological model with a Gauss-Bonnet term in the action. The evolution of the scale factor of the extra dimension (whose dynamics is influenced by the Gauss-Bonnet term) acts as the cause for the breaking of conformal invariance. Different cases have been investigated, each of which is characterized by the number of higher dimensions, the value of the Gauss-Bonnet parameter, and the cosmological constant. Many of the scenarios considered are highly constrained by the requirements that the cosmic evolution is stable, that the normal dimensions expand and that there is no back reaction due to growing electric fields. However there do exist scenarios which satisfy the above requirements and are well suited for magnetogenesis. In particular, a scenario where the number of extra dimensions D = 4 and the cosmological constant is non-zero, turns out to be best suited for generating primordial magnetic fields. It is shown that for these values of parameters, a scale invariant magnetic field of the order of 10 −10 − 10 −9 G can be produced. Even in these most favorable scenarios, the higher dimensional space expands during inflation at the same rate as the normal dimension. Hence if a mechanism could freeze the evolution of the higher dimension, this seems to be a viable mechanism to produce acceptable primordial magnetic fields.

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Section: Magnetogenesis In Gauss-bonnet Gravitymentioning

confidence: 94%

Cosmological magnetogenesis from extra-dimensional Gauss-Bonnet gravity

et al. 2014

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“…We shall study an example in which we take as an initial spacetime a 5D Minkowski described with the cartesian coordinates φ( p) = (t, x, y, z, l) p , in which the tensor metric is given by the orthonormal matrix η AB (26). We choose a IB which is not coordinated, and the struc- N /l, 1), so that we obtain the metric…”

Section: An Example: Monopoles From a 5d Minkowski Spacetime With Conmentioning

confidence: 99%

“…Notice that the spatial components of the magnetic currents decay with time in the Weitzenböck representation. The study of the dynamics for the field fluctuations during de Sitter inflation in the framework of Gravito-electromagnetic Inflation (GEMI) was studied with detail in [25,26], and this goes beyond the scope of this paper. However, as has been demonstrated in (43), from the point of view of the Levi-Civita representation there are no currents related to gravito-magnetic sources.…”

Section: An Example: Monopoles From a 5d Minkowski Spacetime With Conmentioning

confidence: 99%

Gravito-magnetic currents in the inflationary universe from WIMT

Romero

Bellini

2014

Eur. Phys. J. C

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Using the Weitzenböck representation of a Riemann-flat 5D spacetime, we study the possible existence of primordial gravito-magnetic currents from Gravitoelectromagnetic Inflation (GEMI). We found that these currents decrease exponentially in the Weitzenböck representation, but they are null in a Levi-Civita representation because we are dealing with a 5D Riemann-flat spacetime without structure or torsion.

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The evolution of primordial magnetic fields since their generation

2016

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We study the evolution of primordial magnetic fields in an expanding cosmic plasma. For this purpose we present a comprehensive theoretical model to consider the evolution of MHD turbulence that can be used over a wide range of physical conditions, including cosmological and astrophysical applications. We model different types of decaying cosmic MHD turbulence in the expanding universe and characterize the large-scale magnetic fields in such a medium. Direct numerical simulations of freely decaying MHD turbulence are performed for different magnetogenesis scenarios: magnetic fields generated during cosmic inflation as well as electroweak and QCD phase transitions in the early universe.Magnetic fields and fluid motions are strongly coupled due to the high Reynolds number in the early universe. Hence, we abandon the simple adiabatic dilution model to estimate magnetic field amplitudes in the expanding universe and include turbulent mixing effects on the large-scale magnetic field evolution. Numerical simulations have been carried out for non-helical and helical magnetic field configurations. The numerical results show the possibility of inverse transfer of energy in magnetically dominated non-helical MHD turbulence. On the other hand, decay properties of helical turbulence depend on whether the turbulent magnetic field is in a weakly or a fully helical state.Our results show that primordial magnetic fields can be considered as a seed for the observed large-scale magnetic fields in galaxies and clusters. Bounds on the magnetic field strength are obtained and are consistent with the upper and lower limits set by observations of extragalactic magnetic fields. * Electronic address: tinatin@andrew.cmu.edu † Electronic address: Axel.Brandenburg@Colorado.edu ‡ Electronic address: aleko@tevza.org

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Seminal magnetic fields from inflato-electromagnetic inflation

Cited by 4 publications

References 59 publications

Cosmological magnetogenesis from extra-dimensional Gauss-Bonnet gravity

Cosmological magnetogenesis from extra-dimensional Gauss-Bonnet gravity

Gravito-magnetic currents in the inflationary universe from WIMT

The evolution of primordial magnetic fields since their generation

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