Measuring the neutron star compactness and binding energy with supernova neutrinos

Abstract : 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.
Type de document :
Article dans une revue
JCAP, 2017, 11 (11), pp.036. 〈10.1088/1475-7516/2017/11/036〉
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Soumis le : mercredi 20 décembre 2017 - 23:55:44
Dernière modification le : mercredi 24 octobre 2018 - 03:20:03

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Andrea Gallo Rosso, Francesco Vissani, Maria Volpe. Measuring the neutron star compactness and binding energy with supernova neutrinos. JCAP, 2017, 11 (11), pp.036. 〈10.1088/1475-7516/2017/11/036〉. 〈hal-01669663〉



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