Turbulent Thermalization

By R. Micha, Igor I. Tkachev. 2004

208 citations recorded by the source corpus.

We study, analytically and with lattice simulations, the decay of coherent ﬁeld oscillations and the subsequent thermalization of the resulting stochastic classical wave-ﬁeld. The problem of reheating of the Universe after inﬂation constitutes our prime motivation and application of the results. We identify three diﬀerent stages of these processes. During the initial stage of “parametric resonance”, only a small fraction of the initial inﬂaton energy is transferred to ﬂuctuations in the physically relevant case of suﬃciently large couplings. A major fraction is transfered in the prompt regime of driven turbulence. The subsequent long stage of thermalization classiﬁes as free turbulence. During the turbulent stages, the evolution of particle distribution functions is self-similar. We show that wave kinetic theory successfully describes the late stages of our lattice calculation. Our analytical results are general and give estimates of reheating time and temperature in terms of coupling constants and initial inﬂaton amplitude.

Subfields: Astronomy and Astrophysics, Finance, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/50297b63f3febeb33e0ff8326bde00054e8dc6ea

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Citations in the corpus

Inflation and string cosmology (2001, methodology): “These particles interact with each other and come to a state of thermal equilibrium with some temperature Tr [13, 14, 15, 16, 17, 18, 19].”
Schwinger mechanism revisited (2015, background): “cent of the quantum nature of the process under consideration. Similar equations to eqs. (135) and (137) for the particle production by parametric resonance in a ˚4 scalar theory can be found in ref. [63]. In this seemingly unrelated problem, the large zero mode of the eld acts as a time dependent b”
Standard Model—axion—seesaw—Higgs portal inflation. Five problems of particle physics and cosmology solved in one stroke (2016, background): “This is the process of turbulent thermalisation described in [160,161], with the difference that in our case the inflaton is a complex field.”
Early seeds of axion miniclusters (2018, background): “s (those with L= 12;20 converge much better at low-k). cut-o, where there is a vast deciency of axions. These dynamics can be probably understood in terms of the turbulent thermalisation mechanisms [76]. The spectrum tends to a self-similar solution, that allows the transfer of particle number to re”
Reheating in Inflationary Cosmology: Theory and Applications (2010, methodology): “The period when the intial re-scatterings take place and which ends when the turbulent scaling distribution becomes established is longer than the period of the intial resonance, but not by a large factor [11].”