Constraints on the scalar-field potential in warm inflation

Montefalcone, Gabriele; Aragam, Vikas; Visinelli, Luca; Freese, Katherine

doi:10.48550/arxiv.2209.14908

Cited by 3 publications

(6 citation statements)

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“…For this, a strictly positive coefficient c > 0 for the temperature dependence of the dissipation rate leads to a negative correlation between λ φ and the parameter Q, implying that for large values of the dissipation strength Q the constraint in eq. (2.24) is significantly tighter than in cold inflation [15].…”

Section: Jcap03(2023)002mentioning

confidence: 72%

“…This was derived at first in ref. [14] for standard cold inflation and recently generalized for a strongly dissipative regime to be [15]:…”

Section: Jcap03(2023)002mentioning

confidence: 99%

“…which is in fact always < 1 as long as b G > − 9 2 . 15 This motivates the possibility to study the c = −1 case in the strong regime of warm inflation and for a significantly sub-Planckian value of f . This however will require an extension of the range of validity of the growth factor G(Q) for the c = −1 case previously derived in ref.…”

Section: Summary and Future Outlookmentioning

confidence: 99%

“…[14] in the context of cold inflation models and generalized by ref. [15] to warm inflation, potentials must be extremely flat for rolling models of inflation. The potential must be wide enough to sustain a sufficient number of e-folds of inflation (typically 60), while its height is restricted in scale in order to not overproduce density perturbations from quantum fluctuations.…”

Section: Introductionmentioning

confidence: 99%

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Observational constraints on warm natural inflation

Montefalcone

Aragam

Visinelli

et al. 2023

J. Cosmol. Astropart. Phys.

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Warm natural inflation is studied for the case of the original cosine potential. The radiation bath during inflation induces a dissipation (friction) rate in the equation of motion for the inflaton field, which can potentially reduce the field excursion needed for an observationally viable period of inflation. We examine if the dissipation thus provides a mechanism to avoid the large decay constant f ≳ M pl of cold cosine natural inflation. Whereas temperature independent dissipation has previously been shown to alleviate the need for a trans-Planckian decay constant f, we illustrate here the difficulties of accommodating a significantly sub-Planckian decay constant (f < 10-1 M pl) for the case of a temperature dependent dissipation rate in the form Γ ∝ Tc , with c = {1,3}. Such dissipation rates represent physically well-motivated constructions in the literature. For each model, we map its location in the r-ns plane and compare with cosmic microwave background (CMB) data. For c = 1 (c = 3), we find that agreement with CMB data requires that dissipation be in the weak (moderate) regime and that the minimum allowed value of the decay constant in the potential is f min = 0.3 (0.8) M pl, respectively.

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Section: Jcap03(2023)002mentioning

confidence: 72%

“…This was derived at first in ref. [14] for standard cold inflation and recently generalized for a strongly dissipative regime to be [15]:…”

Section: Jcap03(2023)002mentioning

confidence: 99%

Section: Summary and Future Outlookmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Observational constraints on warm natural inflation

Montefalcone

Aragam

Visinelli

et al. 2023

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…Moreover, there are several papers in the literature which studied WI using some quasi-de Sitter form of scale factor, e.g., intermediate and logamediate inflation, and other noncanonical versions of field theory, e.g., tachyonic fields, in the high dissipative regime [117][118][119][120][121][122][123][124][125], while there have been also many studies involving different forms of inflaton potentials and in other interesting contexts [79,111,[126][127][128][129][130][131][132][133][134][135][136][137][138][139][140][141][142][143][144].…”

Section: B Other Applications and Recent Results In Wimentioning

confidence: 99%

Recent developments in warm inflation

Kamali¹,

Motaharfar²,

Ramos³

2023

Preprint

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Warm inflation, its different particle physics model implementations and the implications of dissipative particle production for its cosmology are reviewed. First, we briefly present the background dynamics of warm inflation and contrast it with the cold inflation picture. An exposition of the space of parameters for different well-motivated potentials, which are ruled out, or severely constrained in the cold inflation scenario, but not necessarily in warm inflation, is provided. Next, the quantum field theory aspects in realizing explicit microscopic models for warm inflation are given. This includes the derivation of dissipation coefficients relevant in warm inflation for different particle field theory models. The dynamics of cosmological perturbations in warm inflation are then described. The general expression for the curvature scalar power spectrum is shown. We then discuss in details the relevant regimes of warm inflation, the weak and strong dissipative regimes. We also discuss the results predicted in these regimes of warm inflation and how they are confronted with the observational data. We explain how the dissipative dynamics in warm inflation can address several long-standing issues related to (post-) inflationary cosmology. This includes recent discussions concerning the so-called swampland criteria and how warm inflation can belong to the landscape of string theory.

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Recent Developments in Warm Inflation

2023

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Warm inflation, its different particle physics model implementations, and the implications of dissipative particle production for its cosmology are reviewed. First, we briefly present the background dynamics of warm inflation and contrast it with the cold inflation picture. An exposition of the space of parameters for different well-motivated potentials, which are ruled out, or severely constrained in the cold inflation scenario, but not necessarily in warm inflation, is provided. Next, the quantum field theory aspects in realizing explicit microscopic models for warm inflation are given. This includes the derivation of dissipation coefficients relevant in warm inflation for different particle field theory models. The dynamics of cosmological perturbations in warm inflation are then described. The general expression for the curvature scalar power spectrum is shown. We then discuss in detail the relevant regimes of warm inflation, the weak and strong dissipative regimes. We also discuss the results predicted in these regimes of warm inflation and how they are confronted with the observational data. We explain how the dissipative dynamics in warm inflation can address several long-standing issues related to (post-) inflationary cosmology. This includes recent discussions concerning the so-called swampland criteria and how warm inflation can belong to the landscape of string theory.

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Constraints on the scalar-field potential in warm inflation

Cited by 3 publications

References 0 publications

Observational constraints on warm natural inflation

Observational constraints on warm natural inflation

Recent developments in warm inflation

Recent Developments in Warm Inflation

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