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Nuclear matter
About: Nuclear matter is a research topic. Over the lifetime, 10180 publications have been published within this topic receiving 248261 citations.
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TL;DR: In this article, a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and β-stable nuclear matter at zero temperature was derived in the framework of chiral perturbation theory.
Abstract: Aims. We report a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and β -stable nuclear matter at zero temperature using recent realistic two-body and three-body nuclear interactions derived in the framework of chiral perturbation theory (ChPT) and including the Δ(1232) isobar intermediate state. This EOS is provided in tabular form and in parametrized form ready for use in numerical general relativity simulations of binary neutron star merging. Here we use our new EOS for β -stable nuclear matter to compute various structural properties of non-rotating neutron stars.Methods. The EOS is derived using the Brueckner–Bethe–Goldstone quantum many-body theory in the Brueckner–Hartree–Fock approximation. Neutron star properties are next computed solving numerically the Tolman–Oppenheimer–Volkov structure equations. Results. Our EOS models are able to reproduce the empirical saturation point of symmetric nuclear matter, the symmetry energy E sym , and its slope parameter L at the empirical saturation density n 0 . In addition, our EOS models are compatible with experimental data from collisions between heavy nuclei at energies ranging from a few tens of MeV up to several hundreds of MeV per nucleon. These experiments provide a selective test for constraining the nuclear EOS up to ~4n 0 . Our EOS models are consistent with present measured neutron star masses and particularly with the mass M = 2.01 ± 0.04 M ⊙ of the neutron stars in PSR J0348+0432.
77 citations
TL;DR: In this paper, the authors study the hadron-quark phase transition in the interior of neutron stars and find that the maximum masses are never larger than 1.6 solar masses, no matter the model chosen for describing the pure quark phase.
Abstract: We study the hadron-quark phase transition in the interior of neutron stars (NS). For the hadronic sector, we use a microscopic equation of state (EOS) involving nucleons and hyperons derived within the Brueckner-Bethe-Goldstone many-body theory, with realistic two-body and three-body forces. For the description of quark matter, we employ both the MIT bag model with a density dependent bag constant, and the color dielectric model. We calculate the structure of NS interiors with the EOS comprising both phases, and we find that the NS maximum masses are never larger than 1.6 solar masses, no matter the model chosen for describing the pure quark phase.
77 citations
TL;DR: In this paper, a case study and status report of proton-nucleus scattering at medium energies is presented, which covers existing data for angular distributions of differential cross sections, polarizations, analysing powers, polarization and analysing power differences and spin-flip probabilities between 122 and 400 MeV.
76 citations
TL;DR: In this article, the authors investigated the properties of collapsed stars in the context of another class of quark-matter models that has recently been proposed and concluded that stable quark stars are possible (compare with refs 6, 8, 9).
Abstract: THE possibility of a phase transition between nuclear matter and quark matter has been discussed in recent work1–13. Free quarks would presumably appear above a critical density pq, which is greater than the typical density ρn ≃ 2.5 × 1014g cm−3 within ordinary atomic nuclei. Such a transition might allow stable collapsed stars to exist wherein much of the matter is in the form of quark matter (quark stars). The maximum masses of collapsed stars have been investigated for the extreme case of ρq ≃ ρn and hard equations of state for quark matter5. However, it has been argued6,8,9 that some equations of state for quark matter require ρq >> ρn and are therefore unlikely to permit the existence of stable quark stars. We investigate here the properties of collapsed stars in the context of another class of quark-matter models that has recently been proposed11–13. These models12, which are consistent with all experimental nuclear and high-energy physics data, are based on a quantum chromodynamic treatment of quarks that are assumed to be of low mass (≲100 MeV for the lightest quarks). We find that stable quark stars are possible (compare with refs 6, 8, 9). However, we also conclude (compare with refs 5, 14) that such stars need not have significantly different macroscopic properties from those of neutron-star models15–17 based on conventional nuclear-matter equations of state.
76 citations
TL;DR: In this article, the authors investigated generalized Skyrme-type forces with a term that is both density and momentum-dependent, and proposed a new version of this latter force giving a much better fit to the masses of neutron-rich nuclei.
76 citations