The symmetry energy contribution to the nuclear equation of state impacts various phenomena in nuclear astrophysics, nuclear structure, and nuclear reactions. Its determination is a key objective of contemporary nuclear physics, with consequences for the understanding of dense matter within neutron stars. We examine the results of laboratory experiments that have provided initial constraints on the nuclear symmetry energy and on its density dependence at and somewhat below normal nuclear matter density. Even though some of these constraints have been derived from properties of nuclei while others have been derived from the nuclear response to electroweak and hadronic probes, within experimental uncertainties-they are consistent with each other. We also examine the most frequently used theoretical models that predict the symmetry energy and its slope parameter. By comparing existing constraints on the symmetry pressure to theories, we demonstrate how contributions of three-body forces, which are essential ingredients in neutron matter models, can be determined.

We study the consequences of the hadron-quark deconfinement phase transition in stellar compact objects when finite size effects between the deconfined quark phase and the hadronic phase are taken into account. We show that above a threshold value of the central pressure (gravitational mass) a neutron star is metastable to the decay (conversion) to a hybrid neutron star or to a strange star. The mean-life time of the metastable configuration dramatically depends on the value of the stellar central pressure. We explore the consequences of the metastability of "massive" neutron stars and of the existence of stable compact quark stars (hybrid neutron stars or strange stars) on the concept of limiting mass of compact stars. We discuss the implications of our scenario on the interpretation of the stellar mass and radius extracted from the spectra of several X-ray compact sources. Finally, we show that our scenario implies, as a natural consequence a two step-process which is able to explain the inferred "delayed" connection between supernova explosions and GRBs, giving also the correct energy to power GRBs.

The possibility to draw links between the isospin properties of nuclei and the structure of compact stars is a stimulating perspective. In order to pursue this objective on a sound basis, the correlations from which such links can be deduced have to be carefully checked against model dependence. Using a variety of nuclear effective models and a microscopic approach, we study the relation between the predictions of a given model and those of a Taylor density development of the corresponding equation of state: this establishes to what extent a limited set of phenomenological constraints can determine the core-crust transition properties. From a correlation analysis, we show that (a) the transition density ρt is mainly correlated with the symmetry energy slope L, (b) the proton fraction Yp,t with the symmetry energy and symmetry energy slope (J, L) defined at saturation density, or, even better, with the same quantities defined at ρ = 0.1 fm −3 , and (c) the transition pressure Pt with the symmetry energy slope and curvature (L, Ksym) defined at ρ = 0.1 fm −3 .

We perform a systematic analysis of the density dependence of the nuclear symmetry energy within the microscopic Brueckner-Hartree-Fock (BHF) approach using the realistic Argonne V18 nucleon-nucleon potential plus a phenomenological three body force of Urbana type. Our results are compared thoroughly to those arising from several Skyrme and relativistic effective models.The values of the parameters characterizing the BHF equation of state of isospin asymmetric nuclear matter fall within the trends predicted by those models and are compatible with recent constraints coming from heavy ion collisions, giant monopole resonances or isobaric analog states.In particular we find a value of the slope parameter L = 66.9 MeV, compatible with recent experimental constraints from isospin diffusion, L = 88 ± 25 MeV. The correlation between the neutron skin thickness of neutron-rich isotopes and the slope, L, and curvature, K sym , parameters of the symmetry energy is studied. Our BHF results are in very good agreement with the correlations already predicted by other authors using non-relativistic and relativistic effective models. The correlations of these two parameters and the neutron skin thickness with the transition density from non-uniform to β-stable matter in neutron stars are also analyzed. Our results confirm that there is an inverse correlation between the neutron skin thickness and the transition density.PACS numbers: 21.65.Cd; 21.65.Ef; 21.65.Mn 2 A well-grounded understanding of the properties of isospin-rich nuclear matter is a necessary ingredient for the advancement of both nuclear physics and astrophysics. Isospin asymmetric nuclear matter is present in nuclei, especially in those far away from the stability line, and in astrophysical systems, particularly in neutron stars. A major scientific effort is being carried out at an international level to study experimentally the properties of asymmetric nuclear systems. Laboratory measurements, such as those running or planned to run in the existing or the next-generation, radioactive ion beam facilities at CSR (China), FAIR (Germany), RIKEN (Japan), SPIRAL2/GANIL (France) and the upcoming FRIB (USA), can probe the behavior of the symmetry energy close and above saturation density [1]. Moreover, the 208 Pb Radius Experiment (PREX), scheduled to run at JLab in early 2010, should provide a very accurate measurement of the neutron skin thickness in lead via parity violating electron scattering [2]. Astrophysical observations of compact objects are also a window into both the bulk and the microscopic properties of nuclear matter at extreme isospin asymmetries [3]. The symmetry energy determines to a large extent the composition of β-stable matter and therefore the structure and mass of a neutron star [4].The empirical knowledge gathered from all these sources should be helpful in identifying the major issues arising when the isospin content of nuclear systems is altered. Reliable theoretical investigations of neutron-rich (and possibly proton-rich) systems are...

PACS 13.75.Ev -Hyperon-nucleon interactions PACS 26.60.Kp -Equations of state of neutron-star matter PACS 26.60.-c -Nuclear matter aspects of neutron stars PACS 97.60.Jd -Neutron stars

In this work we review the role of hyperons on the properties of neutron and proto-neutron stars. In particular, we revise the so-called "hyperon puzzle", go over some of the solutions proposed to tackle it, and discuss the implications that the recent measurements of unusually high neutron star masses have on our present knowledge of hypernuclear physics. We reexamine also the role of hyperons on the cooling properties of newly born neutron stars and on the so-called r-mode instability. PACS

We determine the structure of neutron stars within a Brueckner-Hartree-Fock approach based on realistic nucleon-nucleon, nucleon-hyperon, and hyperon-hyperon interactions. Our results indicate rather low maximum masses below 1.4 solar masses. This feature is insensitive to the nucleonic part of the EOS due to a strong compensation mechanism caused by the appearance of hyperons and represents thus strong evidence for the presence of nonbaryonic "quark" matter in the interior of heavy stars. The only way to obtain information on the structure and properties of baryonic matter at extreme densities of several times normal nuclear matter density ρ 0 ≈ 0.17 fm −3 seems to be the theoretical modelling of neutron stars, the unique environment where such densities are actually reached in nature, and the subsequent confrontation with observational data. Any given equation of state (EOS) of baryonic matter determines uniquely the mass-radius relation of neutron star sequences and in particular the maximum mass a neutron star can achieve before collapsing into a black hole.Most theoretical investigations performed so far point to an important feature of high-density β-stable matter, namely that hyperons will appear at densities of about 2, . . . , 3 ρ 0 and strongly soften the EOS. The main consequence is a substantial reduction of the maximum mass [1]. This seems to be an inevitable feature of any approach taking into account the hyperons, caused simply by the availability of additional degrees of freedom of the matter at high density. Any theoretical study of neutron stars without allowing for the presence of hyperons is therefore unrealistic.Evidently it is then important to carry out microscopic calculations as precisely as possible in order to make reliable predictions for the maximum mass of a neutron star composed of baryonic matter and the eventual confrontation with observational data. In this work we report on recent results following this motivation. We try to present strong evidence that the maximum mass of baryonic neutron stars is very low and that therefore neutron stars with larger masses (above ca. 1.5 solar masses) must necessarily contain quark matter.Our theoretical framework is the nonrelativistic BruecknerHartree-Fock (BHF) approach based on microscopic nucleonnucleon (NN), nucleon-hyperon (NY), and hyperon-hyperon (YY) potentials that are fitted to scattering phase shifts, where possible. Nucleonic three-body forces (TBF) are included in order to (slighty) shift the saturation point of purely nucleonic matter to the empirical value.It has been demonstrated that the theoretical basis of the BHF method, the hole-line expansion, is well founded: the nuclear EOS can be calculated with good accuracy in the BHF two hole-line approximation with the continuous choice for the single-particle potential, since the results in this scheme are quite close to the full convergent calculations which include also the three hole-line contribution [2]. Due to these facts, combined with the absence of adjustable parameter...

We present results from Brueckner-Hartree-Fock calculations for ␤-stable neutron star matter with nucleonic and hyperonic degrees of freedom, employing the most recent parametrizations of the baryon-baryon interaction of the Nijmegen group. It is found that the only strange baryons emerging in ␤-stable matter up to total baryonic densities of 1.2 fm Ϫ3 are ⌺ Ϫ and ⌳. The corresponding equations of state are then used to compute properties of neutron stars such as masses and radii.