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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 three-phase model of strongly interacting matter was considered, where each phase was treated as an ideal gas modified by a simple phenomenological interaction feature for nuclear matter, taking into account the baryonic repulsion.
Abstract: We consider a three-phase model of strongly interacting matter, treating each phase as an ideal gas modified by a simple phenomenological interaction feature For nuclear matter, we take into account the baryonic repulsion; for the quark-gluon plasma, we include the bag pressure; the constituent quark phase has a non-zero effective quark mass as well as an independent bag pressure By studying which phase dominates thermodynamically in what region of temperature and baryon number density, we obtain a phase diagram for strongly interacting matter and gain some insight on the relation between deconfinement and chiral symmetry restoration
75 citations
TL;DR: In this paper, a nuclear interaction in chiral effective field theory with explicit inclusion of the Δ-isobar Δ(1232) degree of freedom at all orders up to next-to-next-toleading order (NNLO) was constructed.
Abstract: We construct a nuclear interaction in chiral effective field theory with explicit inclusion of the Δ-isobar Δ(1232) degree of freedom at all orders up to next-to-next-to-leading order (NNLO). We use pion-nucleon (πN) low-energy constants (LECs) from a Roy-Steiner analysis of πN scattering data, optimize the LECs in the contact potentials up to NNLO to reproduce low-energy nucleon-nucleon scattering phase shifts, and constrain the three-nucleon interaction at NNLO to reproduce the binding energy and point-proton radius of He4. For heavier nuclei we use the coupled-cluster method to compute binding energies, radii, and neutron skins. We find that radii and binding energies are much improved for interactions with explicit inclusion of Δ(1232), while Δ-less interactions produce nuclei that are not bound with respect to breakup into α particles. The saturation of nuclear matter is significantly improved, and its symmetry energy is consistent with empirical estimates.
75 citations
TL;DR: In this paper, the occurrence of pairing instability in hot asymmetric nuclear matter was studied within a t-matrix approach, and the thermodynamic tmatrix was solved in the ladder approximation using a realistic nucleon-nucleon potential.
75 citations
TL;DR: In this paper, the sensitivity of the stellar moment of inertia to the neutron-star matter equation of state is examined using accurately calibrated relativistic mean-field models, and it is shown that constraining the density dependence of the symmetry energy -through, for example, the measurement of the neutron skin thickness in {sup 208}Pb - will place no significant bound on either the transition pressure or the crustal moment of gravity.
Abstract: The sensitivity of the stellar moment of inertia to the neutron-star matter equation of state is examined using accurately calibrated relativistic mean-field models. We probe this sensitivity by tuning both the density dependence of the symmetry energy and the high-density component of the equation of state, properties that are at present poorly constrained by existing laboratory data. Particularly attractive is the study of the fraction of the moment of inertia contained in the solid crust. Analytic treatments of the crustal moment of inertia reveal a high sensitivity to the transition pressure at the core-crust interface. This may suggest the existence of a strong correlation between the density dependence of the symmetry energy and the crustal moment of inertia. However, no correlation was found. We conclude that constraining the density dependence of the symmetry energy - through, for example, the measurement of the neutron skin thickness in {sup 208}Pb - will place no significant bound on either the transition pressure or the crustal moment of inertia.
74 citations
TL;DR: In this article, the authors investigated the properties of mixed stars formed by hadronic and quark matter in the framework of relativistic mean field theory, using the nonlinear Walecka model for the hadron matter and the MIT Bag and the Nambu-Jona-Lasinio (NJL) models for the quark mass.
Abstract: We investigate the properties of mixed stars formed by hadronic and quark matter in $\ensuremath{\beta}$ equilibrium described by appropriate equations of state (EOS) in the framework of relativistic mean-field theory We use the nonlinear Walecka model for the hadron matter and the MIT Bag and the Nambu-Jona-Lasinio (NJL) models for the quark matter The phase transition to a deconfined quark phase is investigated In particular, we study the dependence of the onset of a mixed phase and a pure quark phase on the hyperon couplings, quark model, and properties of the hadronic model We calculate the strangeness fraction with baryonic density for the different EOS With the NJL model the strangeness content in the mixed phase decreases The calculations were performed for $T=0$ and for finite temperatures in order to describe neutron and proto-neutron stars The star properties are discussed Both the Bag model and the NJL model predict a mixed phase in the interior of the star Maximum allowed masses for proto-neutron stars are larger for the NJL model $(\ensuremath{\sim}{19M}_{\ensuremath{\bigodot}})$ than that for the Bag model $(\ensuremath{\sim}{16M}_{\ensuremath{\bigodot}})$
74 citations