Primordial Gravitational Waves and the Swampland

Dias, Mafalda; Frazer, Jonathan; Retolaza, Ander; Westphal, Alexander

doi:10.48550/arxiv.1807.06579

Cited by 19 publications

(27 citation statements)

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“…It was readily realised after the recently proposed Swampland Criteria [7] that these criteria regarding formulation of UV-complete low-energy EFTs might have severe consequences for the cosmological epochs relying on de Sitter vacuum, like inflation and dark energy [8]. Since then a series of papers has been written to counter such stumbling blocks and to put both inflation and dark energy back on track, a non-exhaustive list of such analysis would include [16][17][18][19][20][21][40][41][42]. The paper [21] enlists all the possible single-field slow-roll scenarios which are in accordance with the second Swampland Criterion and points out that Warm Inflation is the best option amongst all as far as one considers Swampland Criterion II.…”

Section: Discussionmentioning

confidence: 99%

Warm inflation in the light of swampland criteria

Das

2019

Phys. Rev. D

112

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Warm Inflation seems to be the most befitting single-field slow-roll inflation scenario in the context of the recently proposed Swampland Criteria. We investigate the constraints these Swampland Criteria impose on Warm Inflation parameters and show that Warm Inflation is in accordance with both the current cosmological observations and the proposed Swampland Criteria in both weak and strong dissipative regimes depending on the value of the parameter c which limits the slope of the inflaton potential according to the criteria.

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Section: Discussionmentioning

confidence: 99%

Warm inflation in the light of swampland criteria

Das

2019

Phys. Rev. D

112

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“…The required lower bound on the e-folding number is in tension with the Swampland distance conjecture since it heavily restricts the duration of the inflation [20,35,43]. By using the Swampland distance criterion and the Lyth bound [70] we connect the field variance ∆φ and the total e-folding number N e as follows:…”

Section: Discussionmentioning

confidence: 99%

“…Lastly we emphasize that the precise values of c and D depend on the detailed string construction and they can be slightly larger or smaller than unity [43]. In the following sections, we study if eternal inflation can be realized while satisfying the above two swampland conjectures.…”

Section: Swampland Distance/de Sitter Conjecturesmentioning

confidence: 99%

Eternal inflation and swampland conjectures

Matsui

Takahashi

2019

Phys. Rev. D

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We study if eternal inflation is realized while satisfying the recently proposed string Swampland criteria concerning the range of scalar field excursion, |∆φ| < D · MP, and the potential gradient, |∇V | > c · V /MP, where D and c are constants of order unity, and MP is the reduced Planck mass. We find that only the eternal inflation of chaotic type is possible for c ∼ O(0.01) and 1/D ∼ O(0.01), and that the Hubble parameter during the eternal inflation is parametrically close to the Planck scale, and is in the range of 2πc H inf /MP < 1/ √ 3.[1] A. A. Starobinsky, Phys. Lett. B91, 99 (1980).[2] A. H. Guth, Phys. Rev. D23, 347 (1981).

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“…This means we have M 2 P V ′′ /V < −0.01 when the field value is non-zero during inflation. However, this is in strong tension with the proposal c ′ ∼ 1, although the precise value of c ′ may depend on the detailed string construction and it may be slightly deviate from unity along the line of argument given in [12]. Thus I conclude that hilltop quartic inflation model is incompatible with the refined swampland criteria and type I hilltop inflation model is in tension with it.…”

Section: Conclusion and Discussionmentioning

confidence: 69%