Probing axions with the neutrino signal from the next galactic supernova

TL;DR

This paper investigates how axion emission affects neutrino signals from galactic supernovae, proposing that neutrino observations could constrain axion properties and complement laboratory searches.

Contribution

It introduces a model incorporating axion emission into supernova simulations and assesses the potential for neutrino detectors to detect axion-induced cooling effects.

Findings

Axion emission shortens protoneutron star cooling time.

Neutrino detectors can probe axion masses above 8×10^{-3} eV.

Supernova neutrino observations can complement axion searches like IAXO.

Abstract

We study the impact of axion emission in simulations of massive star explosions, as an additional source of energy loss complementary to the standard neutrino emission. The inclusion of this channel shortens the cooling time of the nascent protoneutron star and hence the duration of the neutrino signal. We treat the axion-matter coupling strength as a free parameter to study its impact on the protoneutron star evolution as well as on the neutrino signal. We furthermore analyze the observability of the enhanced cooling in current and next-generation underground neutrino detectors, showing that values of the axion mass $m_a \gtrsim 8 \times 10^{-3}$ eV can be probed. Therefore a galactic supernova neutrino observation would provide a valuable possibility to probe axion masses in a range within reach of the planned helioscope experiment, the International Axion Observatory (IAXO).