Preheating in Palatini Higgs inflation

Rubio, Javier; Tomberg, Eemeli

doi:10.1088/1475-7516/2019/04/021

Cited by 118 publications

(177 citation statements)

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“…[93] for a recent review on metric Higgs inflation and Refs. [14,22,30,32,36,39,42,43,46,47,53] for recent studies on Palatini-Higgs inflation. The model is specified by…”

Section: Higgs Inflationmentioning

confidence: 99%

“…In principle, because the SM field content and couplings are known, the details of (p)reheating can be calculated exactly, which then gives the total number of e-folds between the end of inflation and horizon exit of the scale where measurements are made[39,43,99,100]. However, in practice the SM couplings are not exactly known, and neither is the Beyond-the-Standard-Model (BSM) physics which accommodates e.g.…”

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confidence: 99%

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Tracing the high energy theory of gravity: an introduction to Palatini inflation

Tenkanen

2020

Gen Relativ Gravit

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We present an introduction to cosmic inflation in the context of Palatini gravity, which is an interesting alternative to the usual metric theory of gravity. In the latter case only the metric g µν determines the geometry of space-time, whereas in the former case both the metric and the space-time connection Γ λ µν are a priori independent variables -a choice which can lead to a theory of gravity different from the metric one. In scenarios where the field(s) responsible for cosmic inflation are coupled non-minimally to gravity or the gravitational sector is otherwise extended, assumptions of the underlying gravitational degrees of freedom can have a big impact on the observational consequences of inflation. We demonstrate this explicitly by reviewing several interesting and well-motivated scenarios including Higgs inflation, R 2 inflation, and ξ-attractor models. We also discuss some prospects for future research and argue why r = 10 −3 is a particularly important goal for future missions that search for signatures of primordial gravitational waves.

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“…[93] for a recent review on metric Higgs inflation and Refs. [14,22,30,32,36,39,42,43,46,47,53] for recent studies on Palatini-Higgs inflation. The model is specified by…”

Section: Higgs Inflationmentioning

confidence: 99%

mentioning

confidence: 99%

Tracing the high energy theory of gravity: an introduction to Palatini inflation

Tenkanen

2020

Gen Relativ Gravit

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“…Setting therefore u = 0 and working in the unitary gauge, H † = (0, h/ √ 2), (86) is actually the model described by g, M 2 and quartic potential as given in (85). The Higgs coupling to gravity and its role as the inflaton, in the metric formulation, has been proposed in [75,76] and it has been widely studied since then [29,32,33,36,38,44, both in the context of the metric formulation and in Palatini formulation. The importance of the R 2 term in (86) has been discussed in [32,33,36,38].…”

Section: B Non-minimally Coupled Modelsmentioning

confidence: 99%

“…These couplings are different in the two approaches. This has been first pointed out in [13] and has attracted the interest of many authors since, , with still continuing activity, [43][44][45][46][47][48][49].…”

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confidence: 99%

Reheating in R2 Palatini inflationary models

Gialamas

Lahanas

2020

Phys. Rev. D

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We consider R 2 inflation in the Palatini gravity assuming the existence of scalar fields, coupled to gravity in the most general manner. These theories, in the Einstein frame, and for one scalar field h, share common features with K -inflation models. We apply this formalism for the study of popular inflationary models, whose potentials are monomials, V ∼ h n , with n a positive even integer. We also study the Higgs model non-minimally coupled to gravity. Although these have been recently studied, in the framework of the Palatini approach, we show that the scalar power spectrum severely constrains these models. Although we do not propose a particular reheating mechanism, we show that the quadratic ∼ h 2 and the Higgs model can survive these constraints with a maximum reheating temperature as large as ∼ 10 15 GeV , when reheating is instantaneous. However, this can be only attained at the cost of a delicate fine-tuning of couplings. Deviations from this fine-tuned values can still yield predictions compatible with the cosmological data, for couplings that lie in very tight range, giving lower reheating temperatures.

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“…However, as expected from earlier studies, the dynamics is highly sensitive to (1) the existence of the kinetic term in the original frame [49], (2) the existence of other degrees of freedom (e.g. whether the inflaton is real or complex [49][50][51], or whether the scalaron degree of freedom exists or not [22,52,53]), (3) the choice of formulations [54], and so on. All of these need further investigation, but are beyond the scope of the present paper.…”

Section: Observational Predictionsmentioning

confidence: 74%