Axions from cooling compact stars: Pair-breaking processes

Once formed in a supernova explosion, a neutron star cools rapidly via neutrino emission during the first image of its life-time. Here we compute the axion emission rate from baryonic components of a star at temperatures below their respective critical temperatures image for normal–superfluid phase transition. The axion production is driven by a charge neutral weak process, associated with Cooper pair breaking and recombination. The requirement that the axion cooling does not overshadow the neutrino cooling puts a lower bound on the axion decay constant image, with image. This translates into an upper bound on the axion mass image.