U(1) symmetric α-attractors

Yamada, Yusuke

doi:10.1007/jhep04(2018)006

Cited by 12 publications

(27 citation statements)

References 51 publications

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“…This result is valid for all models with hyperbolic geometry (1.1) and an unbroken or slightly broken U (1) symmetry, for any α O(1) [1]. In supergravity such models were known only for α = 1/3, but recently such models were constructed for all α < 1 [24], so now we have a broad class of supergravity models with the double attractor behavior found in [1].…”

Section: Introductionmentioning

confidence: 58%

Hypernatural inflation

Linde

Wang

Welling

et al. 2018

J. Cosmol. Astropart. Phys.

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We construct a model of natural inflation in the context of α-attractor supergravity, in which both the dilaton field and the axion field are light during inflation, and the inflaton may be a combination of the two. The T-model version of this theory is defined on the Poincaré disk with radius |Z| = 1. It describes a Mexican hat potential with the flat axion direction corresponding to a circle of radius |Z| < 1. The axion decay constant f a in this theory can be exponentially large because of the hyperbolic geometry of the Poincaré disk. Depending on initial conditions, this model may describe α-attractor inflation driven by the radial component of the inflaton field, natural inflation driven by the axion field, or a sequence of these two regimes. We also construct the E-model version of this theory, which have similar properties. In addition, we describe generalized α-attractor models where the potential can be singular at the boundary of the moduli space, and show that they can provide a simple solution for the problem of initial conditions for the models with plateau potentials.

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Section: Introductionmentioning

confidence: 58%

Hypernatural inflation

Linde

Wang

Welling

et al. 2018

J. Cosmol. Astropart. Phys.

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“…The correlation function can be evaluated by using a dual 3-form gauge theory. Such 3-form gauge theories in (3 + 1) dimensions have been considered in many contexts, e.g., quantum chromodynamics [30][31][32][33][34][35], the strong CP problem [36,37], the cosmological constant problem [33,[38][39][40][41][42][43], inflationary models [37,[44][45][46][47][48][49][50][51][52], string effective theories [53][54][55][56][57][58][59][60][61], supersymmetric field theories (see Refs. [87][88][89] as a review).…”

Section: Introductionmentioning

confidence: 99%

Emergent discrete 3-form symmetry and domain walls

2020

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We show that axion models with the domain wall number k in (3 + 1) dimensions, i.e., periodic scalar field theories admitting k axion domain walls, exhibit an emergent Z k 3-form symmetry for k > 1 in addition to a conventional Z k 0-form symmetry. The emergent 3-form symmetry is explicitly shown by establishing a low-energy dual transformation between the scalar field theory and a 3-form gauge theory. We further argue that the emergent 3-form symmetry is spontaneously broken, and the breaking pattern is so-called the type-B spontaneous symmetry breaking. We discuss similar and different points between the phase admitting the domain walls and topologically ordered phases. * hidaka@riken.jp † nitta@phys-h.keio.ac.jp ‡ ryokokur@post.kek.jp 1 In a spin system, a topologically ordered phase due to the domain wall condensation has been discussed [29].

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“…2 Note that these two Kähler potentials are related via the holomorphic relation Φ = T −1 T +1 and a Kähler transformation (see e.g. [12,13] A classic example of the importance of this type of bound is provided by natural inflation [19], where a single axion in a shift-symmetric potential is responsible for the cosmological dynamics. In the effective field theory description, the axionic shift-symmetry protects the potential from radiative corrections such that large periodicities, i.e.…”

Section: Introductionmentioning

confidence: 99%

Pole N-flation

Dias

Frazer

Retolaza

et al. 2019

J. High Energ. Phys.

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A second order pole in the scalar kinetic term can lead to a class of inflation models with universal predictions referred to as pole inflation or α-attractors. While this kinetic structure is ubiquitous in supergravity effective field theories, realising a consistent UV complete model in e.g. string theory is a non-trivial task. For one, one expects quantum corrections arising in the vicinity of the pole which may spoil the typical attractor dynamics. As a conservative estimate of the range of validity of supergravity models of pole inflation we employ the weak gravity conjecture (WGC). We find that this constrains the accessible part of the inflationary plateau by limiting the decay constant of the axion partner. For the original single complex field models, the WGC does not even allow the inflaton to reach the inflationary plateau region. We analyze if evoking the assistance of N scalar fields from the open string moduli helps addressing these problems. Pole N -flation could improve radiative control by reducing the required range of each individual field. However, the WGC bound prohibiting pole inflation for a single such field persists even for a collective motion of N such scalars if we impose the sublattice WGC. Finally, we outline steps towards an embedding of pole N-flation in type IIB string theory on fibred Calabi-Yau manifolds.

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U(1) symmetric α-attractors

Cited by 12 publications

References 51 publications

Hypernatural inflation

Hypernatural inflation

Emergent discrete 3-form symmetry and domain walls

Pole N-flation

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