Dynamical breaking of shift symmetry in supergravity-based inflation

Mazumdar, Anupam; Noumi, Toshifumi; Yamaguchi, Masahide

doi:10.1103/physrevd.90.043519

Cited by 13 publications

(7 citation statements)

References 45 publications

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“…Actually, the non-minimal kinetic mixing and gravitational coupling of the inflaton can be elegantly realized introducing an approximate shift symmetry [25,[29][30][31][39][40][41][42][43][44][45][46][47][48]. Namely, the constants c − and c + introduced above can be interpreted as the coefficients of the principal shift-symmetric term (c − ) and its violation (c + ) in the Kähler potentials K. Allowing also for a variation of the coefficients of the logarithms appearing in the K's we end up with the most general form of these models analyzed in Reference [26].…”

Section: +0026mentioning

confidence: 99%

Gravitational Waves, μ Term and Leptogenesis from B − L Higgs Inflation in Supergravity

Pallis

2018

Universe

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Abstract:We consider a renormalizable extension of the minimal supersymmetric standard model endowed by an R and a gauged B − L symmetry. The model incorporates chaotic inflation driven by a quartic potential, associated with the Higgs field which leads to a spontaneous breaking of U(1) B−L , and yields possibly detectable gravitational waves. We employ quadratic Kähler potential with a prominent shift-symmetric part proportional to c − and a tiny violation, proportional to c + , included in a logarithm with prefactor −N < 0. An explanation of the µ term of the MSSM is also provided, consistently with the low energy phenomenology, under the condition that one related parameter in the superpotential is somewhat small. Baryogenesis occurs via non-thermal leptogenesis which is realized by the inflaton's decay to the lightest or next-to-lightest right-handed neutrino with masses lower than 1.8 × 10 13 GeV. Our scenario can be confronted with the current data on the inflationary observables, the baryon asymmetry of the universe, the gravitino limit on the reheating temperature and the data on the neutrino oscillation parameters, for 0.012 c + /c − 1/N and gravitino as light as 1 TeV.

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Section: +0026mentioning

confidence: 99%

Gravitational Waves, μ Term and Leptogenesis from B − L Higgs Inflation in Supergravity

Pallis

2018

Universe

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“…The distance traversed by the inflaton field φ is always sub-Planckian as long as f < 0.68 M P , which means the trans-Planckian problem [15,53,54] is absent. This is a direct consequence of the fact that the R 2 corrections ease the slow-roll conditions for inflation and enable inflation to take place at field values below M P .…”

Section: Observational Constraintsmentioning

confidence: 99%

Natural braneworld inflation in light of recent results from Planck and BICEP2

Neupane

2014

Phys. Rev. D

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In this paper we report on a major theoretical observation in cosmology. We present a concrete cosmological model for which inflation has natural beginning and natural ending. Inflation is driven by a cosine-form potential, V (φ) = Λ 4 (1 − cos(φ/f )), which begins at φ πf and ends at φ = φ end 5f /3. The distance traversed by the inflaton field φ is sub-Planckian. The Gauss-Bonnet term R 2 arising as leading curvature corrections in the action S =Lmatter (where α and λ are constants and M is the five-dimensional Planck mass) plays a key role to terminate inflation. The model generates appropriate tensor-to-scalar ratio r and inflationary perturbations that are consistent with Planck and BICEP2 data. For example, for N * = 50 − 60 and ns ∼ 0.960 ± 0.005, the model predicts that M ∼ 5.64 × 10 16 GeV and r ∼ (0.14 − 0.21) [N * is the number of e-folds of inflation and ns (nt) is the scalar (tensor) spectrum spectral index]. The ratio −nt/r is (13% -24%) less than its value in 4D Einstein gravity, −nt/r = 1/8. The upper bound on the energy scale of inflation V 1/4 = 2.37 × 10 16 GeV (r < 0.27) implies that (−λα) 75 × 10 −5 and Λ < 2.17 × 10 16 GeV, which thereby rule out the case α = 0 (Randall-Sundrum model). The true nature of gravity is holographic as implied by the braneworld realization of string and M theory. The model correctly predicts a late-epoch cosmic acceleration with the dark energy equation of state w DE ≈ −1.

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“…[6,16], and for a different approach, cf. [17]. Since string compactifications on Calabi-Yau (CY) manifolds typically yield an abundance of scalar fields in four dimensions, such as geometric moduli or the axio-dilaton, one may ask whether some of these fields can mitigate the problems of the quadratic inflation model without a stabilizer field.…”

Section: Jhep04(2015)058mentioning

confidence: 99%

Challenges for large-field inflation and moduli stabilization

Buchmüller

Dudas

Heurtier

et al. 2015

J. High Energ. Phys.

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Abstract:We analyze the interplay between Kähler moduli stabilization and chaotic inflation in supergravity. While heavy moduli decouple from inflation in the supersymmetric limit, supersymmetry breaking generically introduces non-decoupling effects. These lead to inflation driven by a soft mass term, m 2 ϕ ∼ mm 3/2 , where m is a supersymmetric mass parameter. This scenario needs no stabilizer field, but the stability of moduli during inflation imposes a large supersymmetry breaking scale, m 3/2 H, and a careful choice of initial conditions. This is illustrated in three prominent examples of moduli stabilization: KKLT stabilization, Kähler Uplifting, and the Large Volume Scenario. Remarkably, all models have a universal effective inflaton potential which is flattened compared to quadratic inflation. Hence, they share universal predictions for the CMB observables, in particular a lower bound on the tensor-to-scalar ratio, r 0.05.

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Dynamical breaking of shift symmetry in supergravity-based inflation

Cited by 13 publications

References 45 publications

Gravitational Waves, μ Term and Leptogenesis from B − L Higgs Inflation in Supergravity

Gravitational Waves, μ Term and Leptogenesis from B − L Higgs Inflation in Supergravity

Natural braneworld inflation in light of recent results from Planck and BICEP2

Challenges for large-field inflation and moduli stabilization

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