Oh, wait, O8 de Sitter may be unstable!

Bena, Iosif; Luca, G. Bruno De; Graña, Mariana; Monaco, Gabriele Lo

doi:10.1007/jhep03(2021)168

Cited by 7 publications

(5 citation statements)

References 55 publications

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“…While being more limited in terms of possible content or ingredients, this approach, if successful, would allow a simpler control of required approximations. In practice, the focus has been on 10d type IIA/B supergravities with

D_{p}

‐branes and orientifold

O_{p}

‐planes, [ 35–77 ] assumed to be in the appropriate classical and perturbative regime (small

g_{s}

, large volume, etc.) to be a low energy effective theory of string theory; that assumption has been further studied in [35,63,65,66,70,75].…”

Section: Introductionmentioning

confidence: 99%

Tachyonic de Sitter Solutions of 10d Type II Supergravities

Andriot

2021

Fortschritte der Physik

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Cosmological models of the early or late universe exhibit (quasi) de Sitter space‐times with different stability properties. Considering models derived from string theory, the swampland program does not provide for now a definite characterisation of this stability. In this work we focus on de Sitter solutions of 10d type II supergravities, candidates for classical de Sitter string backgrounds: surprisingly, all known examples are unstable with ηV<−1. We aim at proving the existence of such a systematic tachyon, and getting formally a bound on the value of ηV. To that end, we develop three methods, giving us various sufficient conditions for having a tachyon upon assumptions, in analogy with de Sitter no‐go theorems. Our analysis eventually indicates the existence of variety of different tachyons, and related bounds on ηV. We use this knowledge to find 10 new de Sitter solutions of type IIB supergravity, that have tachyons of a different kind, higher ηV values and new 6d geometries. One solution even appears to be stable, with however non‐compact extra dimensions.

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D_{p}

‐branes and orientifold

O_{p}

‐planes, [ 35–77 ] assumed to be in the appropriate classical and perturbative regime (small

g_{s}

, large volume, etc.) to be a low energy effective theory of string theory; that assumption has been further studied in [35,63,65,66,70,75].…”

Section: Introductionmentioning

confidence: 99%

Tachyonic de Sitter Solutions of 10d Type II Supergravities

Andriot

2021

Fortschritte der Physik

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“…The issue of dS configurations in string theory has proven to be remarkably challenging, to the extent that the most well-studied constructions [13] have been subject to thorough scrutiny and discussion. We shall not attempt to provide a comprehensive account of this extensive subject and its state of affairs, since our focus in the present case lies on higher-dimensional approaches [14][15][16][107][108][109][110] and, in particular, in the search for new solutions [111][112][113][114][115][116][117][118][119][120][121][122][123]. Specifically, the issue at stake is whether the ingredients provided by string-scale supersymmetry breaking can allow for dS compactifications.…”

Section: De Sitter Cosmology: No-gos and Brane-worldsmentioning

confidence: 99%

Supersymmetry Breaking and Stability in String Vacua: brane dynamics, bubbles and the swampland

Basile

2021

Preprint

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We review some aspects of the dramatic consequences of supersymmetry breaking on string vacua. In particular, we focus on the issue of vacuum stability in tendimensional string models with broken, or without, supersymmetry, whose perturbative spectra are free of tachyons. After formulating the models at stake, we introduce their unified low-energy effective description and present a number of vacuum solutions to the classical equations of motion. In addition, we present a generalization of previous no-go results for de Sitter vacua in warped flux compactifications. Then we analyze the classical and quantum stability of these vacua, studying linearized field fluctuations and bubble nucleation. Then, we describe how the resulting instabilities can be framed in terms of brane dynamics, examining in particular brane interactions, back-reacted geometries and commenting on a brane-world string construction along the lines of a recent proposal. After providing a summary, we conclude with some perspectives on possible future developments.

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“…The warp factor and its determination plays a crucial role in testing some swampland conjectures in specific anti-de Sitter solutions [32,33]. Choosing for it and the dilaton non-standard boundary conditions close to O p sources has lead to debated new de Sitter solutions [34][35][36][37][38]; we come back to this discussion in detail in section 2.2. As here, though on a different background metric, the impact of the warp factor on the Kaluza-Klein spectrum appeared important in [39], as it revealed new light states that could play a critical role in the KKLT scenario [40].…”

Section: Introductionmentioning

confidence: 99%

Warp factor and the gravitational wave spectrum

Andriot¹,

Marconnet²,

Tsimpis³

2021

J. Cosmol. Astropart. Phys.

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A distinct signature of compact extra dimensions would be a Kaluza-Klein tower of gravitational waves. Motivated by this prospect, we compute the corresponding spectrum on a warped toroidal background. We evaluate in particular the impact of the warp factor on the spectrum. To that end, we use the complete warp factor H of standard string compactifications, generated by D-branes and orientifolds, thus connecting to recent works on stringy de Sitter constructions. The problematic region close to an orientifold where H < 0 leads to unphysical tachyonic modes in the spectrum. We develop tools that overcome this difficulty and lead to a tachyon-free spectrum. We show, in particular, that the warp factor can lower the first Kaluza-Klein mass by at least 69%.

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Oh, wait, O8 de Sitter may be unstable!

Cited by 7 publications

References 55 publications

Tachyonic de Sitter Solutions of 10d Type II Supergravities

Tachyonic de Sitter Solutions of 10d Type II Supergravities

Supersymmetry Breaking and Stability in String Vacua: brane dynamics, bubbles and the swampland

Warp factor and the gravitational wave spectrum

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