Increasing temperature toward the completion of reheating

Co, Raymond T.; González, E.; Harigaya, Keisuke

doi:10.1088/1475-7516/2020/11/038

Cited by 34 publications

(54 citation statements)

References 92 publications

(96 reference statements)

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“…In this work we studied the damping of scalar condensate oscillations in the mildly non-linear regime in the formalism that naturally accommodates quantum statistical effects of the thermalised medium where dissipation takes place. Thermal corrections to the damping rate are known to be important for applications in cosmology, in particular for the thermal history of the reheating epoch [20,22,26,75,81,[91][92][93][94][95], or the production of axions [96,97] and sterile neutrinos [98]. Our starting point was the non-local equation of motion (1.2) following from the 2PI-resummed effective action (2.21), derived as a loop expansion and a small field expansion in the 2PI effective action formalism of non-equilibrium quantum field theory.…”

Section: Discussionmentioning

confidence: 99%

Oscillating scalar dissipating in a medium

Drewes

Glavan

et al. 2021

J. High Energ. Phys.

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We study how oscillations of a scalar field condensate are damped due to dissipative effects in a thermal medium. Our starting point is a non-linear and non-local condensate equation of motion descending from a 2PI-resummed effective action derived in the Schwinger-Keldysh formalism appropriate for non-equilibrium quantum field theory. We solve this non-local equation by means of multiple-scale perturbation theory appropriate for time-dependent systems, obtaining approximate analytic solutions valid for very long times. The non-linear effects lead to power-law damping of oscillations, that at late times transition to exponentially damped ones characteristic for linear systems. These solutions describe the evolution very well, as we demonstrate numerically in a number of examples. We then approximate the non-local equation of motion by a Markovianised one, resolving the ambiguities appearing in the process, and solve it utilizing the same methods to find the very same leading approximate solution. This comparison justifies the use of Markovian equations at leading order. The standard time-dependent perturbation theory in comparison is not capable of describing the non-linear condensate evolution beyond the early time regime of negligible damping. The macroscopic evolution of the condensate is interpreted in terms of microphysical particle processes. Our results have implications for the quantitative description of the decay of cosmological scalar fields in the early Universe, and may also be applied to other physical systems.

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Section: Discussionmentioning

confidence: 99%

Oscillating scalar dissipating in a medium

Drewes

Glavan

et al. 2021

J. High Energ. Phys.

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“…This also assumes that the temperature is fixed and thus effects from an evolving temperature (see, e.g., Refs. [75][76][77][78]) are neglected. For phenomenological studies, one in principle can compute the self-energies and proper four-vertex functions for any given model, at least numerically.…”

Section: The Model and The Condensate Equation Of Motionmentioning

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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“…Theories of Higgs Parity suffer from the domain wall problem [81] if the Higgs Parity symmetry breaking occurs after inflation. To avoid the problem requires that the reheating temperature is at most v R ; the constraint is typically stronger since the maximal temperature of the universe is in general higher than the reheating temperature [70,82,83] (see, however, [84]). As we have shown in this paper, the baryon asymmetry can be produced naturally via leptogenesis with the reheating temperature much smaller than v R , especially in the freeze-in cosmology, safely avoiding the domain wall problem.…”

Section: Jhep01(2021)125mentioning

confidence: 99%

Sterile neutrino dark matter and leptogenesis in Left-Right Higgs Parity

Dunsky

Hall

Harigaya

2021

J. High Energ. Phys.

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The standard model Higgs quartic coupling vanishes at (109 − 1013) GeV. We study SU(2)L× SU(2)R× U(1)B−L theories that incorporate the Higgs Parity mechanism, where this becomes the scale of Left-Right symmetry breaking, vR. Furthermore, these theories solve the strong CP problem and predict three right-handed neutrinos. We introduce cosmologies where SU(2)R× U(1)B−L gauge interactions produce right-handed neutrinos via the freeze-out or freeze-in mechanisms. In both cases, we find the parameter space where the lightest right-handed neutrino is dark matter and the decay of a heavier one creates the baryon asymmetry of the universe via leptogenesis. A theory of flavor is constructed that naturally accounts for the lightness and stability of the right-handed neutrino dark matter, while maintaining sufficient baryon asymmetry. The dark matter abundance and successful natural leptogenesis require vR to be in the range (1010− 1013) GeV for freeze-out, in remarkable agreement with the scale where the Higgs quartic coupling vanishes, whereas freeze-in requires vR ≳ 109 GeV. The allowed parameter space can be probed by the warmness of dark matter, precise determinations of the top quark mass and QCD coupling by future colliders and lattice computations, and measurement of the neutrino mass hierarchy.

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Increasing temperature toward the completion of reheating

Cited by 34 publications

References 92 publications

Oscillating scalar dissipating in a medium

Oscillating scalar dissipating in a medium

Dissipation of oscillating scalar backgrounds in an FLRW universe

Sterile neutrino dark matter and leptogenesis in Left-Right Higgs Parity

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