Axions from cooling compact stars: pair-breaking processes
arXiv:1205.6940 · doi:10.1016/j.nuclphysa.2012.11.004
Abstract
Once formed in a supernova explosion, a neutron star cools rapidly via neutrino emission during the first 10^4-10^5 yr of its life-time. Here we compute the axion emission rate from baryonic components of a star at temperatures below their respective critical temperatures T_c 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 f_a > 6 10^9 T_{c9}^{-1} GeV, with T_{c9} = T_c/10^9 K. This translates into a upper bound on the axion mass m_a < 10^{-3} T_{c9} eV.
v1: 8 pages, 1 figure, v2: minor changes, 9 pages, 1 figure, matches published version
References in corpus (5)
- An Improved Experimental Limit on the Electric Dipole Moment of the Neutron
- Rapid Cooling of the Neutron Star in Cassiopeia A Triggered by Neutron Superfluidity in Dense Matter
- Neutrino emission due to Cooper-pair recombination in neutron stars revisited
- Vertex renormalization in weak decays of Cooper pairs and cooling compact stars
- Theory of cooling neutron stars versus observations