2000/09/06 by D. N. Voskresensky, Voskresensky, D. N. · 1 citation
Physics and Astronomy · #Astrophysics #Astrophysics and Cosmic Phenomena #Neutrino #Neutrino Physics Research #Neutron star #Nuclear physics #Physics #Pulsars and Gravitational Waves Research #Stars #astro-ph #nucl-th
paper · pdf · doi:10.48550/arxiv.astro-ph/0009093
published in arXiv (Cornell University) (Cornell University) · Invited talk at Intern. Workshop on Phys. of Neutron Star Interiors, Trento, June 2000; 30 pages
openalex publication_date 2000/09/06 · arxiv created 2000/10/23 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
This review demonstrates that neutrino emission from dense hadronic component in neutron stars is subject of strong modifications due to collective effects in the nuclear matter. With the most important in-medium processes incorporated in the cooling code an overall agreement with available soft X ray data can be easily achieved. With these findings so called "standard" and "non-standard" cooling scenarios are replaced by one general "nuclear medium cooling scenario" which relates slow and rapid neutron star coolings to the star masses (interior densities). In-medium effects take important part also at early hot stage of neutron star evolution decreasing the neutrino opacity for less massive and increasing for more massive neutron stars. A formalism for calculation of neutrino radiation from nuclear matter is presented that treats on equal footing one-nucleon and multiple-nucleon processes as well as reactions with resonance bosons and condensates.