The Ground state of matter at high densities: Equation of state and stellar models
About: This article is published in The Astrophysical Journal.The article was published on 1971-01-01. It has received 1314 citations till now. The article focuses on the topics: Ground state & Equation of state.
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TL;DR: In this article, a model relativistic, many-body, quantum field theory composed of a baryon field, a neutral scalar meson field coupled to the scalar density ψ ψ, and a neutral vector meson fields coupled with the conserved Baryon current i Ψ γλψ is developed.
1,557 citations
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TL;DR: In this article, Buchdahl and Tolman showed that the moment of inertia and the binding energy of a neutron star are nearly universal functions of the star's compactness, which can be understood by considering two analytic, yet realistic, solutions of Einstein's equations.
Abstract: The structure of neutron stars is considered from theoretical and observational perspectives We demonstrate an important aspect of neutron star structure: the neutron star radius is primarily determined by the behavior of the pressure of matter in the vicinity of nuclear matter equilibrium density In the event that extreme softening does not occur at these densities, the radius is virtually independent of the mass and is determined by the magnitude of the pressure For equations of state with extreme softening or those that are self-bound, the radius is more sensitive to the mass Our results show that in the absence of extreme softening, a measurement of the radius of a neutron star more accurate than about 1 km will usefully constrain the equation of state We also show that the pressure near nuclear matter density is primarily a function of the density dependence of the nuclear symmetry energy, while the nuclear incompressibility and skewness parameters play secondary roles In addition, we show that the moment of inertia and the binding energy of neutron stars, for a large class of equations of state, are nearly universal functions of the star's compactness These features can be understood by considering two analytic, yet realistic, solutions of Einstein's equations, by, respectively, Buchdahl and Tolman We deduce useful approximations for the fraction of the moment of inertia residing in the crust, which is a function of the stellar compactness and, in addition, the pressure at the core-crust interface
1,354 citations
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TL;DR: An equation of state (EOS) of neutron star matter, describing both the neutron star crust and the liquid core, is calculated in this paper, based on the eective nuclear interaction SLy of the Skyrme type, which is particularly suitable for the calculation of the properties of very neutron rich matter.
Abstract: An equation of state (EOS) of neutron star matter, describing both the neutron star crust and the liquid core, is calculated. It is based on the eective nuclear interaction SLy of the Skyrme type, which is particularly suitable for the application to the calculation of the properties of very neutron rich matter (Chabanat et al. 1997, 1998). The structure of the crust, and its EOS, is calculated in the T = 0 approximation, and under the assumption of the ground state composition. The crust-core transition is a very weakly rst-order phase transition, with relative density jump of about one percent. The EOS of the liquid core is calculated assuming (minimal) npe composition. Parameters of static neutron stars are calculated and compared with existing observational data on neutron stars. The minimum and maximum masses of static neutron stars are 0:094 M and 2:05 M, respectively. Eects of rotation on the minimum and the maximum mass of neutron stars are briefly discussed.
1,063 citations
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TL;DR: In this article, deconfined quark matter within NJL-type models are reviewed, focusing on the regime of low temperatures and moderate densities, which is not accessible by perturbative QCD.
1,008 citations