Inflationary Universe with Anisotropic Hair

Watanabe, Masa Aki; Kanno, Sugumi; Soda, Jiro

doi:10.1103/physrevlett.102.191302

Cited by 362 publications

(725 citation statements)

References 26 publications

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“…Ref. [48] supports the higher form through the same mechanism as 3 See [39] for models of anisotropic inflation that employ the idea of [38]. 4 See [40] for an early lagrangian formulation of the cosmological medium as a fluid, and for the description of its perturbations in terms of phonons.…”

Section: Introductionmentioning

confidence: 87%

“…We follow the notation of [38] of parametrizing by e α the "average" scale factor (the volume scales as √ −g = e 3α ) and by e σ the anisotropy. In principle, one could also consider anisotropic vevs for the scalar fields, φ i = c i x i , with c i being three different constants.…”

Section: Prolonged Anisotropic Background Solutionmentioning

confidence: 99%

“…This is at the basis of the cosmic no-hair conjecture, according to which inflation is expected to rapidly erase any background anisotropy. (29)) as a function of the number of e-folds (of the average scale factor α) for the model (38), and for an initial approximately equal admixture of the two modes in (37). The analytical solution (37) shows a perfect agreement with the exact one.…”

Section: Prolonged Anisotropic Background Solutionmentioning

confidence: 99%

“…We then use the first equation in (30) to set the initial conditionα in , and evolve numerically the last two equations in (30) (for the choice (38), the initial value α in can be reabsorbed in F 0 , which can then be rescaled away from the system of equations). If eq.…”

Section: Prolonged Anisotropic Background Solutionmentioning

confidence: 99%

“…model for inflationary magnetogenesis [32][33][34] (although this application is highly nontrivial to realize [16,[35][36][37]), while the second one has been used to obtain a prolonged stage of anisotropic inflationary expansion [38]. 3 The f (φ) F 2 mechanism and solid inflation constitute the two only examples known so far of a primordial bispectrum with a nontrivial angular dependence in the squeezed limit.…”

Section: Introductionmentioning

confidence: 99%

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Anisotropy in solid inflation

Bartolo

Matarrese

Peloso

et al. 2013

J. Cosmol. Astropart. Phys.

107

150

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In the model of solid / elastic inflation, inflation is driven by a source that has the field theoretical description of a solid. To allow for prolonged slow roll inflation, the solid needs to be extremely insensitive to the spatial expansion. We point out that, because of this property, the solid is also rather inefficient in erasing anisotropic deformations of the geometry. This allows for a prolonged inflationary anisotropic solution, providing the first example with standard gravity and scalar fields only which evades the conditions of the so called cosmic no-hair conjecture. We compute the curvature perturbations on the anisotropic solution, and the corresponding phenomenological bound on the anisotropy. Finally, we discuss the analogy between this model and the f (φ) F 2 model, which also allows for anisotropic inflation thanks to a suitable coupling between the inflaton φ and a vector field. We remark that the bispectrum of the curvature perturbations in solid inflation is enhanced in the squeezed limit and presents a nontrivial angular dependence, as had previously been found for the f (φ) F 2 model.

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Section: Introductionmentioning

confidence: 87%

Section: Prolonged Anisotropic Background Solutionmentioning

confidence: 99%

Section: Prolonged Anisotropic Background Solutionmentioning

confidence: 99%

Section: Prolonged Anisotropic Background Solutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Anisotropy in solid inflation

Bartolo

Matarrese

Peloso

et al. 2013

J. Cosmol. Astropart. Phys.

107

150

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Inflation and conformal invariance: the perspective from radial quantization

Kehagias

Riotto

2017

Fortschritte der Physik

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According to the dS/CFT correspondence, correlators of fields generated during a primordial de Sitter phase are constrained by three-dimensional conformal invariance. Using the properties of radially quantized conformal field theories and the operator-state correspondence, we glean information on some points. The Higuchi bound on the masses of spin-s states in de Sitter is a direct consequence of reflection positivity in radially quantized CFT 3 and the fact that scaling dimensions of operators are energies of states. The partial massless states appearing in de Sitter correspond from the boundary CFT 3 perspective to boundary states with highest weight for the conformal group. We discuss inflationary consistency relations and the role of asymptotic symmetries which transform asymptotic vacua to new physically inequivalent vacua by generating long perturbation modes. We show that on the CFT 3 side, asymptotic symmetries have a nice quantum mechanics interpretation. For instance, acting with the asymptotic dilation symmetry corresponds to evolving states forward (or backward) in "time" and the charge generating the asymptotic symmetry transformation is the Hamiltonian itself. Finally, we investigate the symmetries of anisotropic inflation and show that correlators of four-dimensional free scalar fields can be reproduced in the dual picture by considering an isotropic three-dimensional boundary enjoying dilation symmetry, but with a nonvanishing vacuum expectation value of the boundary stress-energy momentum tensor.

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Inflation

Calcagni¹

2017

Classical and Quantum Cosmology

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Inflationary Universe with Anisotropic Hair

Cited by 362 publications

References 26 publications

Anisotropy in solid inflation

Anisotropy in solid inflation

Inflation and conformal invariance: the perspective from radial quantization

Inflation

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