Condensate decay in a radiation dominated cosmology

TL;DR

This paper investigates the decay dynamics of a scalar condensate in a radiation-dominated universe, highlighting the inadequacy of simple friction models and providing detailed decay rates relevant for ultralight dark matter.

Contribution

It introduces a quantum field theoretical approach to condensate decay in cosmology, incorporating finite temperature effects and showing the limitations of phenomenological friction models.

Findings

Decay during super-Hubble regime follows a specific exponential form.

Finite temperature effects diminish rapidly during expansion.

Friction models underestimate decay timescales in cosmological settings.

Abstract

We study the decay of a homogeneous condensate of a massive scalar field of mass \emph{m} into massless fields in thermal equilibrium in a radiation dominated cosmology. The model is a \emph{proxy} for the non-equilibrium dynamics of a misaligned axion condensate decaying into radiation. After consistent field quantization in the cosmological background, we obtain the causal equations of motion for a homogeneous condensate including the finite temperature self-energy corrections up to one loop. The dynamical renormalization group is implemented to obtain the time dependent relaxation rate that describes the decay dynamics of the condensate amplitude from stimulated emission and recombination of massless quanta in the medium. It is explicitly shown that a simple friction term in the equation of motion does not describe correctly the decay of the condensate. During the super-Hubble regime, relevant for ultralight dark matter, the condensate amplitude decays as $e^{-\frac{g^2}{10} t^2\,\ln(1/mt)}$. In the sub-Hubble regime the amplitude decays as $e^{-\gamma(t;T(t))/2}$ with $T(t)=T_0/a(t)$, therefore the finite temperature contribution to the decay rate vanishes fast during the expansion. A main conclusion is that a phenomenological friction term is inadequate to describe the decay in the super-Hubble regime, the decay function $\gamma(t)$ is always \emph{smaller} than that from a local friction term as a consequence of the cosmological expansion. For ultra light dark matter, the time scale during which transient dynamics is sensitive to cosmological expansion and a local friction term is inadequate, is much longer. A friction term always \emph{underestimates} the time scale of decay in the sub-Hubble case.