2017/08/31 by Andrea Gallo Rosso, Francesco Vissani, Maria Cristina Volpe · 23 citations
Physics and Astronomy · #Cherenkov detector #Compact space #Energy (signal processing) #Equipartition theorem #Gravitational binding energy #Neutrino #Neutrino Physics Research #Neutron #Neutron star #Particle physics theoretical and experimental studies #Pulsars and Gravitational Waves Research #Supernova #hep-ph
paper · pdf · doi:10.1088/1475-7516/2017/11/036
published in Journal of Cosmology and Astroparticle Physics 2017(11), 036 (Institute of Physics) · 14 pages, 3 figures. Minor corrections implemented in version 2
openalex created_date 2017/08/08 · openalex publication_date 2017/11/21 · arxiv created 2017/11/30 · arxiv updated 2017/12/01 · openalex updated_date 2026/08/06
We investigate the precision with which a neutron star gravitational binding energy can be measured through the supernova neutrino signal, without assuming any prior such as the energy equipartition hypothesis, mean energies hierarchy or constraints on the pinching parameters that characterize the neutrino spectra. We consider water Cherenkov detectors and prove that combining inverse beta decay with elastic scattering on electrons is sufficient to reach 11% precision on the neutron star gravitational binding energy already with Super-Kamiokande. The inclusion of neutral current events on oxygen in the analysis does not improve the precision significantly, due to theoretical uncertainties. We examine the possible impact on the conclusion of further theoretical input and of higher statistics. We discuss the implications of our findings on the properties of the newly formed neutron star, in particular concerning the assessment of the compactness or mass-radius relation.