Abstract
Observational identification of black holes as members of binary systems requires the knowledge of the upper limit on the gravitational mass of a neutron star. We use modern equations of state for neutron star matter, fitted to experimental nucleon-nucleon scattering data and the properties of light nuclei, to calculate, within the framework of Rhoades & Ruffini (1974), the minimum upper limit on a neutron star mass. Regarding the equation of state as valid up to twice nuclear matter saturation density, ρnm, we obtain a secure upper bound on the neutron star mass equal to 2.9 M☉. We also find that in order to reach the lowest possible upper bound of 2.2 M☉, we need to understand the physical properties of neutron matter up to a density of ~4ρnm.
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