Curvaton dynamics revisited

Mukaida, Kyohei; Nakayama, Kazunori; Takimoto, Munehiro

doi:10.1088/1475-7516/2014/06/013

Cited by 12 publications

(19 citation statements)

References 57 publications

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“…The first is perturbative interactions with the thermal background. It is known that for larger values of g (m σ /M P ) 1/4 , these will cause a very fast decay of the homogeneous curvaton, and thus would rule out the model [5,8,22]. However, the full calculation of these processes is complicated and involved [8,[23][24][25][26][27][28].…”

Section: Decay Of the Curvaton Field After Inflationmentioning

confidence: 99%

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Quantifying the `naturalness' of the curvaton model

Lerner¹,

Melville²

2014

J. Cosmol. Astropart. Phys.

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We investigate the probability of obtaining an observable curvature perturbation, using as an example the minimal curvaton-higgs (MCH) model. We determine "probably observable" and "probably excluded" regions of parameter space assuming generic initial conditions and applying a stochastic approach for the curvaton's evolution during inflation. Inflation is assumed to last longer than the N obs ≃ 55 observable e-folds, and the total number of e-folds of inflation determines the particular ranges of parameters that are probable. For the MCH model, these "probably observable" regions always lie within the range 8 × 10 4 GeV ≤ m σ ≤ 2 × 10 7 GeV, where m σ is the curvaton mass, and the Hubble scale at horizon exit is chosen as H * = 10 10 GeV. Because the "probably observable" region depends on the total duration of inflation, information on parameters in the Lagrangian from particle physics and from precision CMB observations can therefore provide information about the total duration of inflation, not just the last N obs e-folds. This method could also be applied to any model that contains additional scalar fields to determine the probability that these scalar fields contribute to the curvature perturbation.

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Section: Decay Of the Curvaton Field After Inflationmentioning

confidence: 99%

“…Some attempts have been made to determine Γ in terms of the particle physics couplings of the model. A specific example is the non-perturbative decay of the curvaton into standard model Higgs bosons [5][6][7][8]; the perturbative case is discussed in [9].…”

Section: Introductionmentioning

confidence: 99%

Quantifying the `naturalness' of the curvaton model

Lerner¹,

Melville²

2014

J. Cosmol. Astropart. Phys.

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“…More recently, a few studies have also begun to explore the importance of dissipation in the dynamics of reheating after inflation [46,[81][82][83][84], assuming it proceeds from a supercooled stage where dissipative dynamics plays a negligible role, and also in the dynamics of a curvaton field [85].…”

Section: Discussionmentioning

confidence: 99%

“…The study of dissipative effects has so far been mostly restricted to the early period of inflation, where dissipation may, in fact, completely change the inflaton dynamics and the associated generation of primordial curvature perturbations [22][23][24][25][26][27][28][29][30][31][32][33]. More recently, a few studies have also begun to explore the importance of dissipation in the dynamics of reheating after inflation [46,[81][82][83][84], assuming it proceeds from a supercooled stage where dissipative dynamics plays a negligible role, and also in the dynamics of a curvaton field [85].…”

Section: Discussionmentioning

confidence: 99%

Fluctuation-dissipation dynamics of cosmological scalar fields

2015

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We show that dissipative effects have a significant impact on the evolution of cosmological scalar fields, leading to friction, entropy production and field fluctuations. We explicitly compute the dissipation coefficient for different scalar fields within the standard model and some of its most widely considered extensions, in different parametric regimes. We describe the generic consequences of fluctuationdissipation dynamics in the postinflationary universe, focusing in particular on friction and particle production, and analyze in detail two important effects. First, we show that dissipative friction delays the process of spontaneous symmetry breaking and may even damp the motion of a Higgs field sufficiently to induce a late period of warm inflation. Along with dissipative entropy production, this may parametrically dilute the abundance of dangerous thermal relics. Second, we show that dissipation can generate the observed baryon asymmetry without symmetry restoration, and we develop in detail a model of dissipative leptogenesis. We further show that this generically leads to characteristic baryon isocurvature perturbations that can be tested with cosmic microwave background observations. This work provides a fundamental framework to go beyond the leading thermal equilibrium semiclassical approximation in addressing fundamental problems in modern cosmology.

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“…This seems challenging for a MSSM flat direction, since it has O(1) gauge couplings. As is shown in [32], such a field is rapidly dissipated into thermal plasma and never dominates the universe. If the curvature perturbation of the universe originates from fluctuations of a subdominant component, the fluctuations must be large and the resultant perturbation is highly non-Gaussian [33], which is incompatible with the observations [2].…”

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confidence: 92%

Cosmic perturbations, baryon asymmetry and dark matter from the minimal supersymmetric standard model

Harigaya,

Yamada

2019

Preprint

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Scalar fields in the minimal supersymmetric standard model may have large field values during inflation. Because of approximate global symmetry, it is plausible that the phase directions of them are nearly massless during inflation and obtain quantum fluctuations, which may be the origin of the cosmic perturbations. If perturbations are produced through Q-ball formation, baryon asymmetry and dark matter can be consistently generated. Significant baryon and dark matter isocurvature perturbations are produced, but they are predicted to nearly compensate each other. The lepton asymmetry is much larger than the baryon asymmetry. The scenario predicts local non-Gaussianity of fNL = 5/3. Implication to the mass spectrum of supersymmetric particles is discussed.

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Curvaton dynamics revisited

Cited by 12 publications

References 57 publications

Quantifying the `naturalness' of the curvaton model

Quantifying the `naturalness' of the curvaton model

Fluctuation-dissipation dynamics of cosmological scalar fields

Cosmic perturbations, baryon asymmetry and dark matter from the minimal supersymmetric standard model

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