Magnetic fields from inflation?

Demozzi, Vittoria; Mukhanov, Viatcheslav; Rubinstein, H.R.

doi:10.1088/1475-7516/2009/08/025

Cited by 302 publications

(519 citation statements)

References 25 publications

Supporting

Mentioning

510

Contrasting

Unclassified

Order By: Relevance

“…4 It should also be noted that here we have discussed backreaction from electric fields with a certain wave mode k. Considering the energy density contributions from all super-horizon modes gives an even more stringent upper bound on H inf . The difficulties with inflationary magnetogenesis have already been pointed out in previous studies, such as [17,22]. 5 In particular, the work [22] derived a generic upper bound on H inf without specifying the time evolution of the mode function.…”

Section: Constraints On Inflationmentioning

confidence: 97%

Primordial magnetic fields from the post-inflationary universe

Kobayashi

2014

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We explore cosmological magnetogenesis in the post-inflationary universe, when the inflaton oscillates around its potential minimum and the universe is effectively dominated by cold matter. During this epoch prior to reheating, large-scale magnetic fields can be significantly produced by the cosmological background. By considering magnetogenesis both during and after inflation, we demonstrate that magnetic fields stronger than 10 −15 G can be generated on Mpc scales without having strong couplings in the theory, or producing too large electric fields that would dominate the universe.

show abstract

Section: Constraints On Inflationmentioning

confidence: 97%

Primordial magnetic fields from the post-inflationary universe

Kobayashi

2014

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…We particularly focus on cosmological scenarios for generating large-scale magnetic fields during the inflationary epoch [21,22]. Inflationary magnetogenesis is generically accompanied by the generation of large electric fields as well [23][24][25][26][27], which gives rise to a current via the Schwinger process. When the induced current becomes large, its backreaction to the Maxwell fields becomes non-negligible and can prevent any further generation of the magnetic fields.…”

Section: Jhep10(2014)166mentioning

confidence: 99%

“…[21][22][23][24][25][26][27][42][43][44][45][46][47][48][49][50][51][52], in order to explain the origin of the large-scale magnetic fields in our universe. In such inflationary magnetogenesis scenarios, the magnetic fields are generically accompanied by the production of even larger electric fields.…”

Section: Constraints On Inflationary Magnetogenesismentioning

confidence: 99%

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Kobayashi

Afshordi

2014

J. High Energ. Phys.

140

226

View full text Add to dashboard Cite

We investigate pair creation by an electric field in four-dimensional de Sitter space. The expectation value of the induced current is computed, using the method of adiabatic regularization. Under strong electric fields the behavior of the current is similar to that in flat space, while under weak electric fields the current becomes inversely proportional to the mass squared of the charged field. Thus we find that the de Sitter space obtains a large conductivity under weak electric fields in the presence of a charged field with a tiny mass. We then apply the results to constrain electromagnetic fields in the early universe. In particular, we study cosmological scenarios for generating large-scale magnetic fields during the inflationary era. Electric fields generated along with the magnetic fields can induce sufficiently large conductivity to terminate the phase of magnetogenesis. For inflationary magnetogenesis models with a modified Maxwell kinetic term, the generated magnetic fields cannot exceed 10 −30 G on Mpc scales in the present epoch, when a charged field carrying an elementary charge with mass of order the Hubble scale or smaller exists in the Lagrangian. Similar constraints from the Schwinger effect apply for other magnetogenesis mechanisms.

show abstract

“…model for inflationary magnetogenesis [32][33][34] (although this application is highly nontrivial to realize [16,[35][36][37]), while the second one has been used to obtain a prolonged stage of anisotropic inflationary expansion [38]. 3 The f (φ) F 2 mechanism and solid inflation constitute the two only examples known so far of a primordial bispectrum with a nontrivial angular dependence in the squeezed limit.…”

Section: Introductionmentioning

confidence: 99%

Anisotropy in solid inflation

Bartolo

Matarrese

Peloso

et al. 2013

J. Cosmol. Astropart. Phys.

104

150

View full text Add to dashboard Cite

In the model of solid / elastic inflation, inflation is driven by a source that has the field theoretical description of a solid. To allow for prolonged slow roll inflation, the solid needs to be extremely insensitive to the spatial expansion. We point out that, because of this property, the solid is also rather inefficient in erasing anisotropic deformations of the geometry. This allows for a prolonged inflationary anisotropic solution, providing the first example with standard gravity and scalar fields only which evades the conditions of the so called cosmic no-hair conjecture. We compute the curvature perturbations on the anisotropic solution, and the corresponding phenomenological bound on the anisotropy. Finally, we discuss the analogy between this model and the f (φ) F 2 model, which also allows for anisotropic inflation thanks to a suitable coupling between the inflaton φ and a vector field. We remark that the bispectrum of the curvature perturbations in solid inflation is enhanced in the squeezed limit and presents a nontrivial angular dependence, as had previously been found for the f (φ) F 2 model.

show abstract

Magnetic fields from inflation?

Cited by 302 publications

References 25 publications

Primordial magnetic fields from the post-inflationary universe

Primordial magnetic fields from the post-inflationary universe

Schwinger effect in 4D de Sitter space and constraints on magnetogenesis in the early universe

Anisotropy in solid inflation

Contact Info

Product

Resources

About