Speaker
Description
One of the important processes leading to neutrino emission from the interior of superfluid neutron stars is the process of neutrino emission during Cooper pairing of neutrons. For instance, its rate is crucial for the explanation of the rapid cooling of the neutron star in the Cassiopeia A supernova remnant (if one assumes that the pair breaking and formation process is responsible for this cooling).
When calculating the neutrino emissivity in this process, it is necessary to correctly consider the self-consistent response of the superfluid condensate. Such an analysis for spin-singlet pairing was carried out by many authors and for the spin-triplet case in a series of works by L.B. Leinson in the long-wavelength limit. All these calculations are based on relatively cumbersome equations within the framework of the Larkin-Migdal-Leggett theory or related approaches. In the present study we show that neutrino emission due to Cooper pair formation can be correctly calculated within a somewhat simpler formalism based on the use of the matrix kinetic equation for a superfluid Fermi system, which automatically respects the vector current conservation.
We also give an update of the latest observational results for the Cassiopeia A neutron star cooling.
The work is supported by RSF # 24-12-00320.
