Axion dark matter from inflation-driven quantum phase transition

TL;DR

This paper introduces a novel inflation-driven quantum phase transition mechanism for axion dark matter production, enabling sufficient abundance even for ultralight axions with lower decay constants, and predicts new experimental signatures.

Contribution

It proposes a new axion production mechanism involving a quantum phase transition driven by inflationary fluctuations coupled to the inflaton, differing from the traditional misalignment scenario.

Findings

Axion power spectrum is modified by a curvature parameter $ppa$ during inflation.

The mechanism allows for axion dark matter with lower decay constants.

Predicted parameter space can be tested by future experiments.

Abstract

We propose a new mechanism to produce axion dark matter from inflationary fluctuations. Quantum fluctuations during inflation are strengthened by a coupling of the axion kinetic term to the inflaton, which we parametrize as an effective curvature $\kappa$ in the axion equation of motion. A nonvanishing curvature breaks the scale invariance of the axion power spectrum, driving a quantum phase transition with $\kappa$ as the order parameter. The axion power spectrum is proportional to the inverse comoving horizon to the power of $\kappa$. For positive $\kappa$ the spectrum gets a red tilt, leading to an exponential enhancement of the axion abundance as the comoving horizon shrinks during inflation. This enhancement allows sufficient axion production to comprise the entire dark matter relic abundance despite the ultralight mass. Our mechanism predicts a significantly different parameter space from the usual misalignment mechanism. It allows for axion-like particle dark matter with a much lower decay constant and thus a larger coupling to Standard Model particles. Much of the parameter space can be probed by future experiments including haloscopes, nuclear clocks, CASPEr, and CMB-S4. We can also generate heavier QCD axion dark matter than the misalignment mechanism.