Lattice Calculation of Non-Gaussian Density Perturbations from the Massless Preheating Inflationary Model

Chambers, Alex; Rajantie, Arttu

doi:10.1103/physrevlett.100.041302

Cited by 85 publications

(36 citation statements)

References 19 publications

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“…For example, one can interchange A and B in Eq. (70) to generate another correct sixth-order symplectic factorization with a different Oðdt 7 Þ residual term.…”

Section: How Do We Choose a Discretization Scheme To Include Metric Pmentioning

confidence: 99%

“…The typical comoving scale of preheating is much smaller than current cosmological scales. However, cosmological-scale comoving curvature fluctuations can also be generated via, e.g., preheating modulated by a field that is light during inflation but becomes heavy at the end of inflation [70][71][72]. Moreover, the stochastic background of gravity waves (GWs) generated during preheating [73][74][75][76][77][78][79][80][81] is, in principle, observable.…”

Section: Introductionmentioning

confidence: 99%

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Art of lattice and gravity waves from preheating

Huang

2011

Phys. Rev. D

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The nonlinear dynamics of preheating after early-Universe inflation is often studied with lattice simulations. In this work I present a new lattice code HLATTICE. It differs from previous publicly available codes in the following three aspects: (i) A much higher accuracy is achieved with a modified sixth-order symplectic integrator; (ii) scalar, vector, and tensor metric perturbations in synchronous gauge and their feedback to the dynamics of scalar fields are all included; (iii) the code uses a projector that completely removes the scalar and vector components defined by the discrete spatial derivatives. Such a generic code can have a wide range of applications. As an example, gravity waves from preheating after inflation are calculated with a better accuracy.

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“…For example, one can interchange A and B in Eq. (70) to generate another correct sixth-order symplectic factorization with a different Oðdt 7 Þ residual term.…”

Section: How Do We Choose a Discretization Scheme To Include Metric Pmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Art of lattice and gravity waves from preheating

Huang

2011

Phys. Rev. D

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“…Particle production of daughter fields via parametric resonance, corresponds in fact, to a non-perturbative, non-linear, and out-ofequilibrium phenomenon. Due to this, the violent excitation of field species via parametric resonance is expected to produce large scalar metric perturbations [37][38][39][40][41][42], and a significant amount of gravitational waves [43][44][45][46][47][48][49][50][51][52][53]. Our aim in this paper is precisely to parametrize the production of gravitational waves (GWs) from parametric resonance in the early Universe 2 .…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave production from preheating: parameter dependence

Figueroa

Torrentí

2017

J. Cosmol. Astropart. Phys.

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Parametric resonance is among the most efficient phenomena generating gravitational waves (GWs) in the early Universe. The dynamics of parametric resonance, and hence of the GWs, depend exclusively on the resonance parameter q. The latter is determined by the properties of each scenario: the initial amplitude and potential curvature of the oscillating field, and its coupling to other species. Previous works have only studied the GW production for fixed value(s) of q. We present an analytical derivation of the GW amplitude dependence on q, valid for any scenario, which we confront against numerical results. By running lattice simulations in an expanding grid, we study for a wide range of q values, the production of GWs in post-inflationary preheating scenarios driven by parametric resonance. We present simple fits for the final amplitude and position of the local maxima in the GW spectrum. Our parametrization allows to predict the location and amplitude of the GW background today, for an arbitrary q. The GW signal can be rather large, as h 2 Ω GW (f p ) 10 −11 , but it is always peaked at high frequencies f p 10 7 Hz. We also discuss the case of spectator-field scenarios, where the oscillatory field can be e.g. a curvaton, or the Standard Model Higgs.1 Note that this differs from the case of Higgs-Inflation [24,25], where the post-inflationary decay of the SM Higgs via parametric resonance [26][27][28][29], belongs to the context of preheating, as the Higgs rather plays there the role of the inflaton, instead of a spectator field.2 Note that we do not consider the case of 'oscillons', which correspond to stable field configurations formed whenever a field oscillates around the minimum of its potential, as long as the potential shape meets certain circumstances, see e.g. [54,55]. For the GW production from oscillons see [56,57].3 There exists nonetheless a parameter-fit analysis of the GW production in Hybrid preheating [49], but this corresponds to a spinodal instability of the daughter field modes, not to parametric resonance.

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“…As the fluctuations generated during reheating remain sub-horizon, they cannot leave an observable imprint at the level of the CMB or LSS [15]. Therefore it is difficult to constrain the reheating era, except in some speculative scenarios [16][17][18][19][20][21][22][23][24][25][26]. Still we can put lower and upper bounds on the reheating temperature from the considerations of primordial nucleosynthesis and the energy scale of inflation [27].…”

Section: Introductionmentioning

confidence: 99%

Reheating constraints on Kähler moduli inflation

2019

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The end of inflation is connected to the standard cosmological scenario through reheating. During reheating, the inflaton oscillates around the minimum of the potential and thus decays into the daughter particles that populate the Universe at later times. Using cosmological evolution for observable CMB scales from the time of Hubble crossing to the present time, we translate the constraint on the spectral index n s from Planck data to the constraint on the reheating scenario in the context of Kähler Moduli Inflation. We find that the details of the potential is irrelevant if the analysis is done strictly within the slow-roll formalism. In addition, we extend the de-facto analysis generally done only for the pivot scale to all the observable scales which crossed the Hubble radius during inflation. We study how the maximum number of e-folds varies for different scales, and the effect of the equation of state and potential parameters.

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Lattice Calculation of Non-Gaussian Density Perturbations from the Massless Preheating Inflationary Model

Cited by 85 publications

References 19 publications

Art of lattice and gravity waves from preheating

Art of lattice and gravity waves from preheating

Gravitational wave production from preheating: parameter dependence

Reheating constraints on Kähler moduli inflation

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