Analytic and numerical study of preheating dynamics

Boyanovsky, D.; Vega, H. J. de; Holman, R.; Salgado, J.

doi:10.1103/physrevd.54.7570

Cited by 231 publications

(471 citation statements)

References 47 publications

Supporting

Mentioning

447

Contrasting

Order By: Relevance

“…Contrary to the vacuum initial conditions, parametric resonance shuts off here by the damping of the oscillations and not due to backreaction as in ref. [8]. Therefore, for small g the influence of parametric resonances is highly suppressed.…”

Section: Evolution Equationsmentioning

confidence: 94%

“…The vanishing of the effective mass is accompanied by the presence of Goldstone bosons out of equilibrium as in [3,8].…”

Section: Intermediate and Late Time Dynamicsmentioning

confidence: 99%

“…Such an analysis has been performed in refs. [3,4,8]. In summary, quadratic and logarithmic divergences are absorbed in the mass term while the coupling constant absorbs a logarithmically divergent piece [4,7].…”

Section: Evolution Equationsmentioning

confidence: 99%

“…After renormalization, taking dimensionless variables and introducing a momentum cutoff, the renormalized energy can be written as [8] …”

Section: Energymentioning

confidence: 99%

“…This resonant effect is negligible for small λ. (Parametric unstabilities are shut off by the backreaction for no particle initial conditions [8][9][10]). …”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Nonequilibrium dynamics in quantum field theory at high density: The “tsunami”

Cao

Vega

2001

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

The dynamics of a dense relativistic quantum fluid out of thermodynamic equilibrium is studied in the framework of the Φ 4 scalar field theory in the large N limit. The time evolution of a particle distribution in momentum space (the tsunami) is computed. The effective mass felt by the particles in such a high density medium equals the tree level mass plus the expectation value of the squared field. The case of negative tree level squared mass is particularly interesting. In such case dynamical symmetry restoration as well as dynamical symmetry breaking can happen. Furthermore, the symmetry may stay broken with vanishing asymptotic squared mass showing the presence of out of equilibrium Goldstone bosons. We study these phenomena and identify the set of initial conditions that lead to each case. We compute the equation of state which turns to depend on the initial state. Although the system does not thermalize, the equation of state for asymptotically broken symmetry is of radiation type. We compute the correlation functions at equal times. The two point correlator for late times is the sum of different terms. One stems from the initial particle distribution. Another term accounts for the out of equilibrium Goldstone bosons created by spinodal unstabilities when the symmetry is asymptotically broken. Both terms are of the order of the inverse of the coupling for distances where causal signals can connect the two points. The contribution of the out of equilibrium Goldstones exhibits scaling behaviour in a generalized sense. 11.15.Pg,11.30.Qc

show abstract

Section: Evolution Equationsmentioning

confidence: 94%

“…The vanishing of the effective mass is accompanied by the presence of Goldstone bosons out of equilibrium as in [3,8].…”

Section: Intermediate and Late Time Dynamicsmentioning

confidence: 99%

Section: Evolution Equationsmentioning

confidence: 99%

“…After renormalization, taking dimensionless variables and introducing a momentum cutoff, the renormalized energy can be written as [8] …”

Section: Energymentioning

confidence: 99%

“…This resonant effect is negligible for small λ. (Parametric unstabilities are shut off by the backreaction for no particle initial conditions [8][9][10]). …”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Nonequilibrium dynamics in quantum field theory at high density: The “tsunami”

Cao

Vega

2001

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

show abstract

Lectures on the Theory of Cosmological Perturbations

Brandenberger

2004

Lecture Notes in Physics

197

246

View full text Add to dashboard Cite

Summary. The theory of cosmological perturbations has become a cornerstone of modern quantitative cosmology since it is the framework which provides the link between the models of the very early Universe such as the inflationary Universe scenario (which yield causal mechanisms for the generation of fluctuations) and the wealth of recent high-precision data on the spectrum of density fluctuations and cosmic microwave anisotropies. In these lectures, I provide an overview of the classical and quantum theory of cosmological fluctuations.Crucial points in both the current inflationary paradigm [1,2] of the early Universe and in proposed alternatives such as the Pre-Big-Bang [3] and Ekpyrotic [4] scenarios are that, first, the perturbations are generated on microscopic scales as quantum vacuum fluctuations, and, second, that via an accelerated expansion of the background geometry (or by a contraction of the background), the wavelengths of the fluctuations become much larger than the Hubble radius for a long period of cosmic evolution. Hence, both Quantum Mechanics and General Relativity are required in order to understand the generation and evolution of fluctuations.As a guide to develop the physical intuition for the evolution of inhomogeneities, I begin with a discussion of the Newtonian theory of fluctuations. applicable at late times and on scales smaller than the Hubble radius. The analysis of superHubble fluctuations requires a general relativistic analysis. I first review the classical relativistic theory of fluctuations, and then discuss their quantization. I conclude with a brief overview of two applications of the theory of cosmological fluctuations: the trans-Planckian "problem" of inflationary cosmology and the current status of the study of the back-reaction of cosmological fluctuations on the background space-time geometry. Most of this article is based on the review [5] to which the reader is referred to for the details omitted in these lecture notes. MotivationAs described in the lectures by Tegmark at this school [6], observational cosmology is currently in its golden years. Using a variety of observational techniques, physicists and astronomers are exploring the large-scale structure of the Universe. The Cosmic Microwave Background (CMB) is the observational window which in recent years has yielded the most information. The anisotropies in the CMB have now been detected on a wide range of angular scales, giving us a picture of the Universe at the time of recombination, the time that the cosmic photons last scattered. Large-scale galaxy redshift

show abstract

Primordial magnetic fields from cosmological phase transitions

Boyanovsky

Vega

Simionato

2003

The Early Universe and the Cosmic Microwave Background: Theory and Observations

Self Cite

View full text Add to dashboard Cite

We study the generation of large scale primordial magnetic fields by a cosmological phase transition during the radiation dominated era. The setting is a theory of N charged scalar fields coupled to an abelian gauge field, that undergoes a phase transition at a critical temperature much larger than the electroweak scale. The dynamics after the transition features two distinct stages: a spinodal regime dominated by linear long-wavelength instabilities, and a scaling stage in which the non-linearities and backreaction of the scalar fields are dominant. This second stage describes the growth of horizon sized domains. We implement a formulation based on the non-equilibrium Schwinger-Dyson equations to obtain the spectrum of magnetic fields that includes the dissipative effects of the plasma. We find that large scale magnetogenesis is efficient during the scaling regime. Charged scalar field fluctuations with wavelengths of the order of the Hubble radius induce large scale magnetogenesis via loop effects. The leading processes are: pair production, pair annihilation and low energy bremsstrahlung, these processes while forbidden in equilibrium are allowed strongly out of equilibrium. The ratio between the energy density on scales larger than L and that in the background radiation r(L, T ) = ρB(L, T )/ρ cmb (T ) is r(L, T ) ∼ 10 −34 at the Electroweak scale and r(L, T ) ∼ 10 −14 at the QCD scale for L ∼ 1 Mpc. The resulting spectrum is insensitive to the magnetic diffusion length and equipartition between electric and magnetic fields does not hold. We conjecture that a similar mechanism could be operative after the QCD chiral phase transition.

show abstract

Analytic and numerical study of preheating dynamics

Cited by 231 publications

References 47 publications

Nonequilibrium dynamics in quantum field theory at high density: The “tsunami”

Nonequilibrium dynamics in quantum field theory at high density: The “tsunami”

Lectures on the Theory of Cosmological Perturbations

Primordial magnetic fields from cosmological phase transitions

Contact Info

Product

Resources

About