Secularly growing loop corrections in scalar wave background

Diatlyk, O.

doi:10.1007/jhep10(2020)027

Cited by 15 publications

(12 citation statements)

References 25 publications

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“…We show that for all generalized alpha-states, except the Out-state, loop corrections grow with time signaling the instability of these states. Similar growth was observed in other backgrounds [24], [12], [25], [26] [27], [21], [28], [29], [23].…”

Section: Discussionsupporting

confidence: 84%

Quantum fields in the future Rindler wedge

Akhmedov,

Bazarov,

Diakonov

2021

Preprint

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We consider interacting massive scalar quantum field theory in the future Rindler wedge. This is a model example of quantum field theory in curved space-time. On this simple example we show how dynamics of correlation functions depends on the choice of initial Cauchy surface, basis of modes and on the choice of initial state build with the use of the corresponding creation and annihilation operators. We show which choice of modes in the future Rindler wedge respects Poincaré symmetry. But we do not restrict our attention only to these modes and the corresponding state.

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Section: Discussionsupporting

confidence: 84%

Quantum fields in the future Rindler wedge

Akhmedov,

Bazarov,

Diakonov

2021

Preprint

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“…6. Consider now loop corrections for a generic choice of modes f p (t) in ( 12) and for the initial values n 0 p = 0 and κ 0 p = 0 in (16). As in the situation described in the section 4, the secular memory contribution may come from the sunset two-loop diagram correction to the Keldysh propagator.…”

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confidence: 98%

“…Then modes f p (t) in ( 12) contain the volume factor, [a(t)] (D−1)/2 . This means that such components of the two-point function (16) as n p and κ p are attributed to the comoving volume, i.e. are always accompanied by the factors of the form [a(t)] D−1 in CF.…”

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confidence: 99%

Curved space equilibration vs. flat space thermalization (a short review)

Akhmedov

2021

Preprint

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We discuss equilibration process in expanding universes as compared to the thermalization process in Minkowski space-time. The final goal is to answer the following question: Is the equilibrium reached before the rapid expansion stops and quantum effects have a negligible effect on the background geometry or stress-energy fluxes in a highly curved early Universe have strong effects on the expansion rate and the equilibrium is reached only after the drastic decrease of the space-time curvature? We argue that consideration of more generic noninvariant states in theories with invariant actions is a necessary ingredient to understand quantum field dynamics in strongly curved backgrounds. We are talking about such states in which correlation functions are not functions of such isometry invariants as geodesic distances, while having correct UV behaviour. The reason to consider such states is the presence of IR secular memory effects for generic time dependent backgrounds, which are totally absent in equilibrium. These effects strongly affect the destiny of observables in highly curved spacetimes.

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“…Other works on backreaction effects in non-oscillating scalar backgrounds in the Yukawa theory are Refs. [28][29][30]. 4 For an excellent complementary understanding to Ref.…”

Section: Introductionmentioning

confidence: 99%

Dissipation of oscillating scalar backgrounds in an FLRW universe

Wang¹,

Ai²

2022

Preprint

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We study particle production from oscillating scalar backgrounds in a spatially flat Friedmann-Lemaître-Robertson-Walker universe using non-equilibrium quantum field theory which fully captures the thermal effects and backreaction effects. To be concrete, we consider a Z 2 -symmetric two-scalar model with quartic interactions. For quasi-harmonic oscillations, we adopt the multi-scale analysis to obtain analytical approximate expressions for the self-consistent evolution of the scalar background and the energy density of the produced particles in terms of the retarded self-energy and retarded proper four-vertex function, whose imaginary parts characterize different condensate decay channels and lead to dissipation. We find that reheating in this model can be complete if the imaginary part of the retarded self-energy is non-vanishing, which causes dissipation only at finite temperature through Landau damping. Our results can be generalized to more complicated models and thus could provide a general framework for studying the perturbative reheating process in the early Universe or perturbative production of Dark Matter from an oscillating inflaton.

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Secularly growing loop corrections in scalar wave background

Cited by 15 publications

References 25 publications

Quantum fields in the future Rindler wedge

Quantum fields in the future Rindler wedge

Curved space equilibration vs. flat space thermalization (a short review)

Dissipation of oscillating scalar backgrounds in an FLRW universe

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