Oppenheimer-Volkoff equation

The spherically symmetric, static star configurations are defined by the well known Tolman-Oppenheimer-Volkoff equations [30] for the mechanical equilibrium of self-gravitating matter (see also [14, 31])... 

Energy release due to (anti)neutrino untrapping. The configurations for the quark stars are obtained by solving the Tolman-Oppenheimer-Volkoff equations for a set of central quark number densities nq for which the stars are stable. In Fig. 13 the configurations for different antineutrino chemical potentials are shown. The equations of state with trapped antineutrinos are softer and therefore this allows more compact configurations. The presence of antineutrinos tends to increase the mass for a given central density. 

The first neutron star model in GR was constructed by Oppenheimer and Volkoff (1939). They derived the equations governing a spherically symmetric stellar equilibrium in GR using a metric of the form... 

Figure 1. The relation between central density and the mass of various degenerate star models. Chandrasekhar s curve is for white dwarfs with a mean molecular weight 2 of atomic mass units. Rudkjobing s curve is the same except for inclusion of the relativistic spin-orbit effects Rudkjobing (1952). The curve labeled Oppenheimer and Volkoff is for a set of neutron star models. The solid line marked Wheeler is a set of models computed with a generalized equation of state, from Cameron (1959).

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