Pre-supernova Ultra-light Axion-like Particles

TL;DR

This paper investigates the production and detection of ultra-light axion-like particles (ALPs) from nearby supernova progenitors, proposing gamma ray observations as a method to constrain ALP properties.

Contribution

It introduces a new approach to detect ultra-light ALPs via gamma ray signals from supernova progenitors, providing potential constraints comparable to SN 1987A limits.

Findings

Gamma ray flux from ALPs could be detectable for ALPs lighter than ~1 neV.

Flux dependence on stellar mass is minor compared to magnetic field uncertainties.

Next-generation gamma ray telescopes could set new constraints on ALPs if supernova progenitors are nearby.

Abstract

We calculate the production of ultra-light axion-like particles (ALPs) in a nearby supernova progenitor. Once produced, ALPs escape from the star and a part of them is converted into photons during propagation in the Galactic magnetic field. It is found that the MeV photon flux that reaches Earth may be detectable by gamma ray telescopes for ALPs lighter than ~1 neV when Betelgeuse undergoes oxygen and silicon burning. The dependence of the gamma ray flux on the stellar mass is much smaller than the uncertainty that originates from the Galactic magnetic field. If ALPs are lighter than ~0.1 neV and the supernova progenitor is close enough to the Solar System, the gamma ray flux is insensitive to the distance d because the ALP-photon conversion probability is proportional to d^2. (Non-)detection of gamma rays from a supernova progenitor with next-generation gamma ray telescopes just after pre-supernova neutrino alerts would lead to an independent constraint on ALP parameters as stringent as a SN 1987A limit.