Renormalization of nonequilibrium dynamics at large<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>N</mml:mi></mml:math>and finite temperature

Baacke, J.; Heitmann, Katrin; Pätzold, Carsten

doi:10.1103/physrevd.57.6406

Cited by 25 publications

(29 citation statements)

References 33 publications

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“…Eventually, the energy stored in the homogeneous inflaton is transferred explosively into the production of particles via spinodal or parametric instabilities. [62][63][64][65][66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81] More precisely, nonlinear phenomena eventually shut off the instabilities and stop inflation. [62][63][64][65][66][67]82,83 All these processes lead to the transition to a radiation-dominated era.…”

Section: 3)mentioning

confidence: 99%

The Effective Theory of Inflation in the Standard Model of the Universe and the Cmb+lss Data Analysis

Boyanovsky

Destri

Vega

et al. 2009

Int. J. Mod. Phys. A

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Inflation is today a part of the Standard Model of the Universe supported by the cosmic microwave background (CMB) and large scale structure (LSS) datasets. Inflation solves the horizon and flatness problems and naturally generates density fluctuations that seed LSS and CMB anisotropies, and tensor perturbations (primordial gravitational waves). Inflation theory is based on a scalar field ϕ (the inflaton) whose potential is fairly flat, leading to a slow-roll evolution. This review focuses on the following new aspects of inflation. We present the effective theory of inflationà la Ginsburg and Landau, in which the inflaton potential is a polynomial in the field ϕ and has the universal formM M Pl is the scale of inflation and N ∼ 60 is the number of e-folds since the cosmologically relevant modes exit the horizon till inflation ends. The slow-roll expansion becomes a systematic 1/N expansion and the inflaton couplings become naturally small as powers of the ratio (M/M Pl ) 2 . The spectral index and the ratio of tensor/scalar fluctuations are ns − 1 = O(1/N ), r = O(1/N ), while the running index turns out to be dns/d ln k = O(1/N 2 ) and therefore can be neglected. The energy scale of inflation M ∼ 0.7 × 10 16 GeV is completely determined by the amplitude of the scalar adiabatic fluctuations. A complete analytic study plus the Monte Carlo Markov chain (MCMC) analysis of the available CMB+LSS data (including WMAP5) with fourth degree trinomial potentials showed: (a) the spontaneous breaking of the ϕ → −ϕ symmetry of the inflaton potential; (b) a lower bound for r in new inflation: r > 0.023 (95% CL) and r > 0.046 (68 CL); (c) the preferred inflation potential is a double-well , even function of the field with a moderate quartic coupling yielding as the most probable values ns 0.964, r 0.051. This value for r is within reach of forthcoming CMB observations. The present data in the effective theory of inflation 3669 Int. J. Mod. Phys. A 2009.24:3669-3864. Downloaded from www.worldscientific.com by YALE UNIVERSITY on 02/02/15. For personal use only. 3670 D. Boyanovsky et al.clearly prefer new inflation. Study of higher degree inflaton potentials shows that terms of degree higher than 4 do not affect the fit in a significant way. In addition, a horizon exit happens for ϕ/[ √ NM Pl ] ∼ 0.9, making higher order terms in the potential w negligible. We summarize the physical effects of generic initial conditions (different from Bunch-Davies) on the scalar and tensor perturbations during slow roll and introduce the transfer function D(k), which encodes the observable initial condition effects on the power spectra. These effects are more prominent in the low CMB multipoles: a change in the initial conditions during slow roll can account for the observed CMB quadrupole suppression. Slow-roll inflation is generically preceded by a short, fast-roll stage. Bunch-Davies initial conditions are the natural initial conditions for the fast-roll perturbations. During fast roll, the potential in the wave equations of curvature and tens...

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Section: 3)mentioning

confidence: 99%

The Effective Theory of Inflation in the Standard Model of the Universe and the Cmb+lss Data Analysis

Boyanovsky

Destri

Vega

et al. 2009

Int. J. Mod. Phys. A

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“…There has been considerable interest in this kind of problem due to its many applications, ranging from the dynamics of condensates in condensed matter physics to the evolution of a inflaton field in inflationary cosmology (for a recent review see [1]). Several methods have been applied to this problem involving analytic and numerical analysis [2][3][4][5][6][7][8][9][10][11][12][13][14] as well as lattice simulations [15,16].…”

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confidence: 99%

Affinity for scalar fields to dissipate

2001

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The zero temperature effective equation of motion is derived for a scalar field interacting with other fields. For a broad range of cases, involving interaction with as few as one or two fields, dissipative regimes are found for the scalar field system. The zero temperature limit constitutes a baseline effect that will be prevalent in any general statistical state. Thus, the results found here provide strong evidence that dissipation is the norm not exception for an interacting scalar field system. For application to inflationary cosmology, this provides convincing evidence that warm inflation could be a natural dynamics once proper treatment of interactions is done. The results found here also may have applicability to entropy production during the chiral phase transition in heavy ion collision. PACS number(s): 98

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“…Some examples are found in [4,5,6,7,8,9,10], [11,12,13,14,15,18]. Some works have already been done concerning the dynamics of non homogeneous configuration in bosonic fields.…”

Section: Introductionmentioning

confidence: 99%

“…The renormalization of the time dependent approach (in continuum spaces) can be done in the same way at zero and finite temperatures as well as out-of-thermodynamical equilibrium [10,19,20]. No additional ultraviolet divergence is found due to temporal evolution of the system or its departure from zero temperature or equilibrium.…”

Section: Vacuum and Renormalizationmentioning

confidence: 99%

“…These equations were generalized for the out of equilibrium (non zero temperature) using different methods in [4,10,12,19,21] and they were studied extensively mainly by means of numerical calculations. The choice of initial conditions is entirely subordinate to the approximation, in the sense that were it not Gaussian one might have to consider three conditions instead of two [23].…”

Section: Gaussian Approximationmentioning

confidence: 99%

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Expanding nonhomogeneous configurations of theλφ4model

Braghin

2001

Phys. Rev. D

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A time dependent variational approach is considered to derive the equations of movement for the λφ 4 model. The temporal evolution of the model is performed numerically in the frame of the Gaussian approximation in a lattice of 1+1 dimensions given non homogeneous initial conditions (like bubbles) for the classical and quantum parts of the field which expands. A schematic model for the initial conditions is presented considering the model at finite fermionic density. The non zero fermionic density may lead either to the restoration of the symmetry or to an even more asymmetric phase. Both kinds of situations are considered as initial conditions and the eventual differences in early time dynamics are discussed.In the early time evolution there is strong energy exchange between the classical and quantum parts of the field as the initial configuration expands. The contribution of the quantum fluctuations is discussed especially in the strong coupling constant limit. The continuum limit is analyzed.

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Renormalization of nonequilibrium dynamics at largeNand finite temperature

Cited by 25 publications

References 33 publications

The Effective Theory of Inflation in the Standard Model of the Universe and the Cmb+lss Data Analysis

The Effective Theory of Inflation in the Standard Model of the Universe and the Cmb+lss Data Analysis

Affinity for scalar fields to dissipate

Expanding nonhomogeneous configurations of theλφ4model

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