Consistency of warm<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>k</mml:mi></mml:math>-inflation

Peng, Zhi-Peng; Yu, Jia-Ning; Zhu, Jian-Yang; Zhang, Xiaomin

doi:10.1103/physrevd.94.103531

Cited by 23 publications

(31 citation statements)

References 29 publications

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“…Analogously, this may also alleviate the need for large (superplanckian) inflaton field values in chaotic inflation models. There are various other features of warm inflation that have been explored in the literature [9][10][11][12][13][14][15][16][17][18][19][20][21][22][23][24][25][26].…”

Section: Introductionmentioning

confidence: 99%

Dynamical and observational constraints on the warm little inflaton scenario

et al. 2018

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We explore the dynamics and observational predictions of the Warm Little Inflaton scenario, presently the simplest realization of warm inflation within a concrete quantum field theory construction. We consider three distinct types of scalar potentials for the inflaton, namely chaotic inflation with a quartic monomial potential, a Higgs-like symmetry breaking potential and a nonrenormalizable plateau-like potential. In each case, we determine the parametric regimes in which the dynamical evolution is consistent for 50-60 e-folds of inflation, taking into account thermal corrections to the scalar potential and requiring, in particular, that the two fermions coupled directly to the inflaton remain relativistic and close to thermal equilibrium throughout the slow-roll regime and that the temperature is always below the underlying gauge symmetry breaking scale. We then compute the properties of the primordial spectrum of scalar curvature perturbations and the tensorto-scalar ratio in the allowed parametric regions and compare them with Planck data, showing that this scenario is theoretically and observationally successful for a broad range of parameter values.

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Section: Introductionmentioning

confidence: 99%

Dynamical and observational constraints on the warm little inflaton scenario

et al. 2018

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“…For a representative list of recent references see Refs. [36][37][38][39][40][41][42][43][44][45]. The dissipative effect arises from a friction term or dissipative coefficient , which describes the processes of the scalar field dissipating into a thermal bath via its interaction with other field degrees of freedom.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of warm power-law plateau inflation with a generalized inflaton decay rate: predictions and constraints after Planck 2015

Jawad¹,

Videla²,

Gulshan³

2017

Eur. Phys. J. C

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In the present work, we study the consequences of considering a new family of single-field inflation models, called power-law plateau inflation, in the warm inflation framework. We consider the inflationary expansion is driven by a standard scalar field with a decay ratio having a generic power-law dependence with the scalar field φ and the temperature of the thermal bath T given by. Assuming that our model evolves according to the strong dissipative regime, we study the background and perturbative dynamics, obtaining the most relevant inflationary observable as the scalar power spectrum, the scalar spectral index and its running and the tensor-toscalar ratio. The free parameters characterizing our model are constrained by considering the essential condition for warm inflation, the conditions for the model evolves according to the strong dissipative regime and the 2015 Planck results through the n s -r plane. For completeness, we study the predictions in the n s -dn s /d ln k plane. The model is consistent with a strong dissipative dynamics and predicts values for the tensor-to-scalar ratio and for the running of the scalar spectral index consistent with current bounds imposed by Planck and we conclude that the model is viable.

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“…where k is the wave number in Fourier space. The Einstein equation of the multi-component system is given by 19)…”

Section: )mentioning

confidence: 99%

Two-field warm inflation and its scalar perturbations on large scales

2018

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We explore the homogeneous background dynamics and the evolution of generated perturbations of cosmological inflation that is driven by multiple scalar fields interacting with a perfect fluid. Then we apply the method to warm inflation driven by two scalar fields and a radiation fluid, and present general results about the evolution of the inflaton and radiation. After decomposing the perturbations into adiabatic and entropy modes, we give the equation of motion of adiabatic and entropy perturbations on large scales. Then, we give numerical results of background and perturbation equations in a concrete model (the dissipative coefficient Γ ∝ H). At last, we use the most recent observational data to constrain our models and give the observationally allowed regions of parameters. This work is a natural extension of warm inflation to multi-field cases.PACS numbers: 98.80.Cq II. MULTI-COMPONENT INFLATIONLet us study the inflation in homogeneous and isotropic background. We consider a spatially flat Friedmann-Robertson-Walker (FRW) metric of the form ds 2 = −dt 2 + a(t) 2 δ ij dx i dx j , (2.1)

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Consistency of warmk-inflation

Cited by 23 publications

References 29 publications

Dynamical and observational constraints on the warm little inflaton scenario

Dynamical and observational constraints on the warm little inflaton scenario

Dynamics of warm power-law plateau inflation with a generalized inflaton decay rate: predictions and constraints after Planck 2015

Two-field warm inflation and its scalar perturbations on large scales

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