Global embedding of fibre inflation models

Cicoli, Michele; Muia, Francesco; Shukla, Pramod

doi:10.1007/jhep11(2016)182

Cited by 58 publications

(113 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(3.27) and we also show some plots that ensure the validity of the approximations performed during this models that do not employ axions [136][137][138]. For such inflationary models explicit string theory embeddings have been built, including a controlled moduli stabilization procedure and the presence of a chiral visible sector [139,140]. 44 In this case the gauge bosons receive string scale masses.…”

Section: B Scalar Power Spectrum and Consistency Checksmentioning

confidence: 84%

PBH dark matter from axion inflation

Domcke

Muia

Pieroni

et al. 2017

J. Cosmol. Astropart. Phys.

Self Cite

107

View full text Add to dashboard Cite

Protected by an approximate shift symmetry, axions are well motivated candidates for driving cosmic inflation. Their generic coupling to the Chern-Simons term of any gauge theory gives rise to a wide range of potentially observable signatures, including equilateral non-Gaussianites in the CMB, chiral gravitational waves in the range of direct gravitational wave detectors and primordial black holes (PBHs). In this paper we revisit these predictions for axion inflation models non-minimally coupled to gravity.Contrary to the case of minimally coupled models which typically predict scale-invariant mass distributions for the generated PBHs at small scales, we demonstrate how broadly peaked PBH spectra naturally arises in this setup. For specific parameter values, all of dark matter can be accounted for by PBHs.Dedicated to the memory of Pierre Binétruy

show abstract

Section: B Scalar Power Spectrum and Consistency Checksmentioning

confidence: 84%

PBH dark matter from axion inflation

Domcke

Muia

Pieroni

et al. 2017

J. Cosmol. Astropart. Phys.

Self Cite

107

View full text Add to dashboard Cite

show abstract

“…Additional KK mode corrections may then arise from the exchange of KK modes with these additional objects [21]. We should therefore expect KK mode corrections of the form displayed in eq.…”

Section: Jhep02(2018)117mentioning

confidence: 99%

“…This will generate winding mode corrections even we only wrap either τ 1 or τ 2 but not both. Therefore, generically the winding mode corrections are expected to be present [21].…”

Section: Jhep02(2018)117mentioning

confidence: 99%

Fibre inflation and α-attractors

Каллош

Linde

Roest

et al. 2018

J. High Energ. Phys.

View full text Add to dashboard Cite

Fibre inflation is a specific string theory construction based on the Large Volume Scenario that produces an inflationary plateau. We outline its relation to α-attractor models for inflation, with the cosmological sector originating from certain string theory corrections leading to α = 2 and α = 1/2. Above a certain field range, the steepening effect of higher-order corrections leads first to the breakdown of single-field slow-roll and after that to the onset of 2-field dynamics: the overall volume of the extra dimensions starts to participate in the effective dynamics. Finally, we propose effective supergravity models of fibre inflation based on an D3 uplift term with a nilpotent superfield. Specific moduli dependent D3 induced geometries lead to cosmological fibre models but have in addition a de Sitter minimum exit. These supergravity models motivated by fibre inflation are relatively simple, stabilize the axions and disentangle the Hubble parameter from supersymmetry breaking.

show abstract

“…without tadpoles) configuration of D3/D7 branes. Several explicit examples are known of this kind of realizations [18]. To stabilize the complex structure moduli and the dilaton, one has to assume that background fluxes are also turned on [36].…”

Section: Fibre Inflation Modelsmentioning

confidence: 99%

“…Both these quantities depend on the equation-of-state parameter w reh (EoS), in an effective description based on a cosmic fluid. In this paper, we want to investigate the constraints on N reh and T reh as functions of the scalar spectral index, n s , focusing on the class of the so-called string fiber inflation models [16][17][18]. It results in a large volume scenario [19] where the inflaton is a Kähler module, and it typically predicts a scalar spectral index n s ∼ 0.97, together with a tensor-to-scalar ratio of the order of r ∼ 0.006 for an inflationary number of e-foldings N * ∼ 60.…”

Section: Introductionmentioning

confidence: 99%

Fiber inflation and reheating

2017

View full text Add to dashboard Cite

We present constraints on the reheating era within the string Fiber Inflation scenario, in terms of the effective equation-of-state parameter of the reheating fluid, w reh . The results of the analysis, completely independent on the details of the inflaton physics around the vacuum, illustrate the behavior of the number of e-foldings during the reheating stage, N reh , and of the final reheating temperature, T reh , as functions of the scalar spectral index, ns. We analyze our results with respect to the current bounds given by the PLANCK mission data and to upcoming cosmological experiments. We find that large values of the equation-of-state parameter (w reh > 1/3) are particularly favored as the scalar spectral index is of the order of ns ∼ 0.9680, with a σn s ∼ 0.002 error. Moreover, we compare the behavior of the general reheating functions N reh and T reh in the fiber Inflation scenario with the one extracted by the class of the α-attractor models with α = 2. We find that the corresponding reheating curves are very similar in the two cases.

show abstract

Global embedding of fibre inflation models

Cited by 58 publications

References 66 publications

PBH dark matter from axion inflation

PBH dark matter from axion inflation

Fibre inflation and α-attractors

Fiber inflation and reheating

Contact Info

Product

Resources

About