Small field polynomial inflation: reheating, radiative stability and lower bound

Drees, Manuel; Xu, Yong

doi:10.1088/1475-7516/2021/09/012

Cited by 25 publications

(32 citation statements)

References 71 publications

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“…It has been recently shown that such a polynomial inflection-point inflationary scenario fits easily consistent with current CMB observations with rather large parameter space [53]. Additionally, the inflationary predictions can be analyzed analytically even though the model includes several free parameters [53]. A notable prediction is that the running of the spectral index α ∼ O(10 −3 ), making this small field inflationary model testable in the near future [54].…”

Section: Introductionmentioning

confidence: 53%

“…The polynomial nature of the inflaton potential is a key difference from the usually considered monomial scenarios, which has been gaining interests since the 1990s [48][49][50][51][52]. In the minimally coupled scenario, the flatness of a polynomial potential of quartic order is guaranteed by the existence of a (near) inflection-point [53]. It has been recently shown that such a polynomial inflection-point inflationary scenario fits easily consistent with current CMB observations with rather large parameter space [53].…”

Section: Introductionmentioning

confidence: 73%

“…In the minimally coupled scenario, the flatness of a polynomial potential of quartic order is guaranteed by the existence of a (near) inflection-point [53]. It has been recently shown that such a polynomial inflection-point inflationary scenario fits easily consistent with current CMB observations with rather large parameter space [53]. Additionally, the inflationary predictions can be analyzed analytically even though the model includes several free parameters [53].…”

Section: Introductionmentioning

confidence: 88%

“…In this section we briefly review SR inflation with focus on the polynomial inflection-point inflation formalism [53]. For b = 9…”

Section: Inflationmentioning

confidence: 99%

“…It is naturally therefore to extend the study presented in Ref. [53] in order to tackle the DM problem.…”

Section: Introductionmentioning

confidence: 98%

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Polynomial Inflation and Dark Matter

Bernal,

2021

Preprint

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We present a minimal UV complete framework to embed inflation and dark matter by extending the standard model with a singlet real scalar field (the inflaton) and a singlet fermonic field acting as dark matter. The inflaton features the most general renormalizable polynomial up to quartic order, which is flat due to the existence of a perturbed inflection-point, comfortably fitting CMB measurements. We also analyze (p)reheating by considering the Higgs production via inflaton decay. In the early universe, dark matter can be generated by the mediation of gravitons or inflatons. However, the production via the direct decay of the inflatons dominates, making viable a large range of dark matter masses, from O(10 −5 ) GeV to O(10 11 ) GeV.

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Section: Introductionmentioning

confidence: 53%

Section: Introductionmentioning

confidence: 73%

Section: Introductionmentioning

confidence: 88%

“…In this section we briefly review SR inflation with focus on the polynomial inflection-point inflation formalism [53]. For b = 9…”

Section: Inflationmentioning

confidence: 99%

“…It is naturally therefore to extend the study presented in Ref. [53] in order to tackle the DM problem.…”

Section: Introductionmentioning

confidence: 98%

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Polynomial Inflation and Dark Matter

Bernal,

2021

Preprint

Self Cite

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Post-inflationary leptogenesis and dark matter production: metric versus Palatini formalism

Ghoshal,

Lalak,

Pal

et al. 2024

J. High Energ. Phys.

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We investigate production of non-thermal dark matter particles and heavy sterile neutrinos from inflaton during the reheating era, which is preceded by a slow-roll inflationary epoch with a quartic potential and non-minimal coupling (ξ) between inflaton and gravity. We compare our analysis between metric and Palatini formalism. For the latter, the tensor-to-scalar ratio, r, decreases with ξ. We find that for ξ = 0.5 and number of e-folds ~ 60, r can be as small as ~ $$ \mathcal{O} $$ O (10−3) which may be validated at future reaches of upcoming CMB observation such as CMB-S4 etc. We identify the permissible range of Yukawa coupling yχ between inflaton and fermionic DM χ, to be $$ \mathcal{O} $$ O (10−3.5) ≳ yχ ≳ $$ \mathcal{O} $$ O (10−20) for metric formalism and $$ \mathcal{O} $$ O (10−4) ≳ yχ ≳ $$ \mathcal{O} $$ O (10−11) for Palatini formalism which is consistent with current PLANCK data and also within the reach of future CMB experiments. For the scenario of leptogenesis via the decay of sterile neutrinos produced from inflaton decay, we also investigate the parameter space involving heavy neutrino mass MN1 and Yukawa coupling yN1 of sterile neutrino with inflaton, which are consistent with current CMB data and successful generation of the observed baryon asymmetry of the universe via leptogenesis. In contrast to metric formalism, in the case of Palatini formalism, for successful leptogenesis to occur, we find that yN1 has a very narrow allowable range and is severely constrained from the consistency with CMB predictions.

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Inflection-point inflation and dark matter redux

Ghoshal

Lambiase

Pal

et al. 2022

J. High Energ. Phys.

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We investigate for viable models of inflation that can successfully produce dark matter (DM) from inflaton decay process, satisfying all the constraints from Cosmic Microwave Background (CMB) and from some other observations. In particular, we analyze near-inflection-point small field inflationary scenario with non-thermal production of fermionic DM from the decaying inflaton field during the reheating era. To this end, we propose two different models of inflation with polynomial potential. The potential of Model I contains terms proportional to linear, quadratic, and quartic in inflaton; whereas in Model II, the potential contains only even power of inflaton and the highest term is sextic in inflaton. For both the models, we find out possible constraints on the model parameters which lead to proper inflationary parameters from CMB data with a very small tensor-to-scalar ratio, as expected from a small-field model. With the allowed parameter space from CMB, we then search for satisfactory relic abundance for DM, that can be produced from inflaton via reheating, to match with the present-day cold dark matter (CDM) relic density for the parameter spaces of the DM χ mass and Yukawa couplings in the range 10−9 ≳ yχ ≳ 10−15 and 103GeV ≲ mχ ≲ 109GeV. The DM relic is associated with the inflection-points in each model via maximum temperature reached in the early universe during its production. Finally, we find out allowed parameter space coming out of combined constraints from stability analysis for both SM Higgs and DM decays from inflaton as well as from BBN and Lyman-α bounds.

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Small field polynomial inflation: reheating, radiative stability and lower bound

Cited by 25 publications

References 71 publications

Polynomial Inflation and Dark Matter

Polynomial Inflation and Dark Matter

Post-inflationary leptogenesis and dark matter production: metric versus Palatini formalism

Inflection-point inflation and dark matter redux

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