2005/07/23 by M. E. Gusakov, A. D. Kaminker, D. G. Yakovlev +1 · 4 citations
Physics and Astronomy · #Equation of state #High-Energy Particle Collisions Research #Neutrino #Neutron #Neutron star #Nucleon #Pairing #Pulsars and Gravitational Waves Research #Scientific Research and Discoveries #Superfluidity #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2005.09459.x
published as Mon.Not.Roy.Astron.Soc.363:555-562, 2005 · 9 pages, 6 figures; accepted for publication in MNRAS
arxiv created 2005/07/23 · openalex publication_date 2005/09/07 · arxiv updated 2014/10/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We study the cooling of superfluid neutron stars whose cores consist of nucleon matter with the Akmal—Pandharipande—Ravenhall (APR) equation of state. This equation of state opens the powerful direct Urca process of neutrino emission in the interior of most massive neutron stars. Extending our previous recent studies (Papers I and II), we employ phenomenological density-dependent critical temperatures Tcp(ρ) of strong singlet-state proton pairing (with the maximum in the outer stellar core) and Tcnt(ρ) of moderate triplet-state neutron pairing (with the maximum in the inner core). Choosing the position of properly, we can obtain a representative class of massive neutron stars whose cooling is intermediate between the cooling enhanced by neutrino emission due to Cooper pairing of neutrons in the absence of the direct Urca process and the very fast cooling provided by the direct Urca process non-suppressed by superfluidity.