Magnetogenesis and the primordial non-gaussianity

Seery, David

doi:10.1088/1475-7516/2009/08/018

Cited by 25 publications

(40 citation statements)

References 120 publications

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“…Finally, by using the relation (10), we find the consistency relation for the magnetic field to be (20) in agreement with (8). With the parametrization in (12), we obtain the consistency relation b N L = n B − 4.…”

supporting

confidence: 71%

Consistency relation for cosmic magnetic fields

Jain

Sloth

2012

Phys. Rev. D

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If cosmic magnetic fields are indeed produced during inflation, they are likely to be correlated with the scalar metric perturbations that are responsible for the Cosmic Microwave Background anisotropies and Large Scale Structure. Within an archetypical model of inflationary magnetogenesis, we show that there exists a new simple consistency relation for the non-Gaussian cross correlation function of the scalar metric perturbation with two powers of the magnetic field in the squeezed limit where the momentum of the metric perturbation vanishes. We emphasize that such a consistency relation turns out to be extremely useful to test some recent calculations in the literature. Apart from primordial non-Gaussianity induced by the curvature perturbations, such a cross correlation might provide a new observational probe of inflation and can in principle reveal the primordial nature of cosmic magnetic fields.

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supporting

confidence: 71%

Consistency relation for cosmic magnetic fields

Jain

Sloth

2012

Phys. Rev. D

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“…Some attempts so far in this direction have been unsuccessful [39], but a general study remains to be done. If this, or some other idea [41], can circumvent the strong coupling problem, our findings provide a signature that may be correlated with the magnetic field.…”

Section: Magnetogenesismentioning

confidence: 75%

“…The work [39] computed instead the cosmological perturbations in the case in which (2) provides scale invariant "magnetic" components of the vector field, as in the magnetogenesis application [25,40]. Cosmological applications in this context have also been studied in [41]. Studies of the cosmological perturbations in [25,40] start from the point of view that the statistics of the generated "magnetic" field is isotropic, and therefore obtain statistical isotropic results.…”

mentioning

confidence: 99%

Anisotropic power spectrum and bispectrum in thef(ϕ)F2mechanism

et al. 2013

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A suitable coupling of the inflaton ϕ to a vector kinetic term F 2 gives frozen and scale invariant vector perturbations. We compute the cosmological perturbations ζ that result from such coupling by taking into account the classical vector field that unavoidably gets generated at large scales during inflation. This generically results in a too anisotropic power spectrum of ζ. Specifically, the anisotropy exceeds the 1% level (10% level) if inflation lasted ∼ 5 e-folds (∼ 50 e-folds) more than the minimal amount required to produce the CMB modes. This conclusion applies, among others, to the application of this mechanism for magnetogenesis, for anisotropic inflation, and for the generation of anisotropic perturbations at the end of inflation through a waterfall field coupled to the vector (in this case, the unavoidable contribution that we obtain is effective all throughout inflation, and it is independent of the waterfall field). For a tuned duration of inflation, a 1% (10%) anisotropy in the power spectrum corresponds to an anisotropic bispectrum which is enhanced like the local one in the squeezed limit, and with an effective local fNL ∼ 3 (∼ 30). More in general, a significant anisotropy of the perturbations may be a natural outcome of all models that sustain higher than 0 spin fields during inflation.

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“…(2.3), which does not resemble the structure of those most popular ones analysed in the literature. There will be some intrinsic non-Gaussianities arising from the third order coupled metric and three-form perturbations [46][47][48], but we expect this contribution to be subdominant, since the direct coupling is strongly enhanced by the rapid development of the vector potential instabilities (which in turn give rise to strong magnetic fields).…”

Section: Non-gaussianitiesmentioning

confidence: 99%