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The QCD axion is a hypothetical particle motivated by the Strong CP problemof particle physics. One of the primary ways in which its existence can beinferred is via its function as an additional cooling channel in stars, withsome of the strongest constraints coming from the supernova observationSN1987A. Multimessenger observations of binary neutron star mergers (such asthose of GW170817, AT2017gfo, and GRB170817A) may provide another scenario inwhich such constraints could be obtained. In particular, the axion couldpotentially alter the lifetime, the ejection of material, and the emittedgravitational wave signal of the postmerger remnant. In this article, weperform numerical relativity simulations of a binary neutron star merger,including a phenomenological description of the nucleon-nucleon-axionbremsstrahlung to quantify the effects of such a cooling channel on thedynamical evolution. While our simulations show a difference in the temperatureprofile of the merger remnant, the imprint of the axion vianucleon-nucleon-axion bremsstrahlung on the emitted gravitational wave signaland the ejecta mass is too small to improve constraints on the axion mass withcurrent or future planned detectors. Whilst we consider a limited number ofcases, and a simplified cooling model, these broadly represent the "best case"scenario, thus, a more thorough investigation is unlikely to change theconclusions, at least for this particular interaction channel.

Cooling binary neutron star remnants via nucleon-nucleon-axion bremsstrahlung