Is the Standard Model in the Swampland? Consistency Requirements from Gravitational Scattering

Aoki, Katsuki; Loc, Tran Quang; Noumi, Toshifumi; Tokuda, Junsei

doi:10.1103/physrevlett.127.091602

Cited by 34 publications

(20 citation statements)

References 31 publications

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“…and all 2d modes whose effective masses are H satisfy the rotating version of the FL bound (although a mass of order Hubble means the corresponding field is close to saturating 7 This is reminiscent of the proposed bound Λ EFT ≤ √ gmMP for pure QED in [33,34]. In this case too the charge carriers provide a (much stronger) upper bound on the EFT cut-off scale, albeit stemming from non-trivial assumptions about the scattering amplitudes.…”

Section: Rotating Black Holesmentioning

confidence: 86%

“…In this case too the charge carriers provide a (much stronger) upper bound on the EFT cut-off scale, albeit stemming from non-trivial assumptions about the scattering amplitudes. Note that the cut-off in [34] is dependent on the complete particle spectrum of the theory and is for instance heavily modified going from QED to electroweak theory.…”

Section: Rotating Black Holesmentioning

confidence: 99%

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The FL bound and its phenomenological implications

Montero

Vafa

Riet

et al. 2021

J. High Energ. Phys.

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Demanding that charged Nariai black holes in (quasi-)de Sitter space decay without becoming super-extremal implies a lower bound on the masses of charged particles, known as the Festina Lente (FL) bound. In this paper we fix the $$ \mathcal{O}(1) $$ O 1 constant in the bound and elucidate various aspects of it, as well as extensions to d > 4 and to situations with scalar potentials and dilatonic couplings. We also discuss phenomenological implications of FL including an explanation of why the Higgs potential cannot have a local minimum at the origin, thus explaining why the weak force must be broken. For constructions of meta-stable dS involving anti-brane uplift scenarios, even though the throat region is consistent with FL, the bound implies that we cannot have any light charged matter fields coming from any far away region in the compactified geometry, contrary to the fact that they are typically expected to arise in these scenarios. This strongly suggests that introduction of warped anti-branes in the throat cannot be decoupled from the bulk dynamics as is commonly assumed. Finally, we provide some evidence that in certain situations the FL bound can have implications even with gravity decoupled and illustrate this in the context of non-compact throats.

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Section: Rotating Black Holesmentioning

confidence: 86%

Section: Rotating Black Holesmentioning

confidence: 99%

The FL bound and its phenomenological implications

Montero

Vafa

Riet

et al. 2021

J. High Energ. Phys.

View full text Add to dashboard Cite

show abstract

“…In the latter, the bounds must be satisfied up to the inclusion of gravitational UV effects, which are typically beyond the range of application of the EFT, but which can violate a strict positivity condition. Positivity bounds in the presence of gravity have been used to study the coupling of matter to gravitation in several models [60][61][62][63], but their application to modified gravity has been mostly restricted to cases were dynamical gravitons are either neglected [64][65][66][67][68] or massive [69,70].…”

Section: Jhep03(2022)075mentioning

confidence: 99%

The shape of scalar Gauss-Bonnet gravity

Herrero-Valea

2022

J. High Energ. Phys.

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We study the consistency of Scalar Gauss-Bonnet Gravity, a generalization of General Relativity where black holes can develop non-trivial hair by the action of a coupling F(Φ)$$ \mathcal{G} $$ G between a function of a scalar field and the Gauss-Bonnet invariant of the space-time. When properly normalized, interactions induced by this term are weighted by a cut-off, and take the form of an Effective Field Theory expansion. By invoking the existence of a Lorentz invariant, causal, local, and unitary UV completion of the theory, we derive positivity bounds for n-to-n scattering amplitudes including exchange of dynamical gravitons. These constrain the value of all even derivatives of the function F(Φ), and are highly restrictive. They require some of the scales of the theory to be of Planckian order, and rule out most of the models used in the literature for black hole scalarization.

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“…For instance, it may be at (10 3 − 10 4 ) GeV [34,35] or (10 14 − 10 16 ) GeV [36] or (0.7 − 1.6)10 15 GeV [37] or (10 13 − 10 15 ) GeV [38]. In this study, we use the cut-off scale Λ ∼ 10 14 GeV [39] and assume that the VEV of singlets are at a very high energy scale:…”

Section: Introductionmentioning

confidence: 99%