Neutrino emission from binary neutron star mergers

Both thermal and non-thermal neutrinos are expected to produce in binary neutron star (BNS) merger events. The thermal neutrino production starts from the tidal disruption during the inspiral phase and peaks at tens of milliseconds after the merging event. If the merger remnant ends up as a short gamma ray burst or a stable magnetar, substantial particle acceleration can occur in the corresponding relativistic shock waves or pulsar wind nebula, resulting in prompt to delayed emissions of (ultra) high energy neutrinos. Therefore, observation of neutrinos from BNS merger events can not only help to dissect the instantaneous and remnant merger environments, decipher the cosmic ray acceleration mechanism, but also can help to study the fundamental properties of neutrinos and search for new physics beyond the Standard Model of particle physics over astronomical baselines.