Gauge fields and inflation

By A. Maleknejad, M. Sheikh-Jabbari, Jiro Soda. 2012

355 citations recorded by the source corpus.

Abstract The isotropy and homogeneity of the cosmic microwave background (CMB) favors “scalar driven” early Universe inflationary models. However, gauge fields and other non-scalar fields are far more common at all energy scales, in particular at high energies seemingly relevant to inflation models. Hence, in this review we consider the role and consequences, theoretical and observational, that gauge fields can have during the inflationary era. Gauge fields may be turned on in the background during inflation, or may become relevant at the level of cosmic perturbations. There have been two main classes of models with gauge fields in the background, models which show violation of the cosmic no-hair theorem and those which lead to isotropic FLRW cosmology, respecting the cosmic no-hair theorem. Models in which gauge fields are only turned on at the cosmic perturbation level, may source primordial magnetic fields. We also review specific observational features of these models on the CMB and/or the primordial cosmic magnetic fields. Our discussions will be mainly focused on the inflation period, with only a brief discussion on the post inflationary (p)reheating era.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a0d67af44420baa64a5b3abd41f47c8597b186d5

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Citations in the corpus

Adding helicity to inflationary magnetogenesis (2014, background): “See [29] for a review on gauge fields during inflation.”
Exploring cosmic origins with CORE: Inflation (2016, background): “Deviations from nt ≈ −r/8 are expected for well motivated extensions of the simplest scalar field inflationary models, which include generalized Lagrangians [210, 211], multifield inflation [212–214], and gauge inflation [215].”
Inflation and String Theory (2014, neutral): “Another recent proposal, which we will now describe in some detail, is that inflation can be achieved by coupling an axion to non-Abelian gauge fields with suitable vevs [625, 797] (see [815–817] and the review article [818] for”
Gauge-preheating and the end of axion inflation (2015, background): “Furthermore, couplings of scalar fields to Abelian [57–59] or non-Abelian gauge fields in cosmological settings have been studied in recent years [60–75].”
Planck2018 results (2018, background): “…et al. 2002; Byrnes & Wands 2006), in the models with generalized Lagrangians (Garriga & Mukhanov 1999; Kobayashi et al. 2010), in gauge inflation (Maleknejad et al. 2013), or in a more radical way in alternative models to inflation (Gasperini & Veneziano 1993; Boyle et al. 2004; Brandenberger et…”