Density dependence of the nuclear symmetry energy from measurements of neutron radii in nuclei

Viñas, X.; Centelles, M.; Roca-Maza, X.; Warda, M.

doi:10.1063/1.4891141

Cited by 5 publications

(3 citation statements)

References 89 publications

(171 reference statements)

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“…It has been a major aim of recent efforts in nuclear physics to determine values for these characteristic parameters of cold nuclear matter from various experiments, see, e.g., the contribution of X. Viñas et al in this volume [43]. Instead of the quantity L, the symmetry pressure p 0 = Ln sat /3 is introduced in some works.…”

Section: Nuclear Mattermentioning

confidence: 99%

Effects of the liquid-gas phase transition and cluster formation on the symmetry energy

et al. 2014

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Abstract. Various definitions of the symmetry energy are introduced for nuclei, dilute nuclear matter below saturation density and stellar matter, which it found in compact stars or core-collapse supernovae. The resulting differences are exemplified by calculations in a theoretical approach based on a generalized relativistic density functional for dense matter. It contains nucleonic clusters as explicit degrees of freedom with medium dependent properties that are derived for light clusters from a quantum statistical approach. With such a model the dissolution of clusters at high densities can be described. The effects of the liquidgas phase transition in nuclear matter and of cluster formation in stellar matter on the density dependence of the symmetry energy are studied for different temperatures. It is observed that correlations and the formation of inhomogeneous matter at low densities and temperatures causes an increase of the symmetry energy as compared to calculations assuming a uniform uncorrelated spatial distribution of constituent baryons and leptons.

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Section: Nuclear Mattermentioning

confidence: 99%

Effects of the liquid-gas phase transition and cluster formation on the symmetry energy

et al. 2014

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“…These observations triggered many theoretical and experimental studies to explore the relation of isospin-dependent properties of nuclei to the EoS, in particular, the density dependence of the nuclear symmetry energy E sym ðnÞ. An extension of the Skyrme HF calculations in similar studies of RMF models (Typel and Brown, 2001), general density functionals in the context of EFT (Furnstahl, 2002) Viñas et al (2014aViñas et al ( , 2014b. The consequences for the properties of NSs, such as radius or proton fraction, were studied by Horowitz and Piekarewicz (2001a, 2002, Steiner et al (2005), Todd-Rutel and , and Avancini et al (2007aAvancini et al ( , 2007bAvancini et al ( , 2007c.…”

Section: Neutron Skin Thicknessesmentioning

confidence: 99%

Equations of state for supernovae and compact stars

et al. 2017

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A review is given of various theoretical approaches for the equation of state (EoS) of dense matter, relevant for the description of core-collapse supernovae, compact stars, and compact star mergers. The emphasis is put on models that are applicable to all of these scenarios. Such EoS models have to cover large ranges in baryon number density, temperature, and isospin asymmetry. The characteristics of matter change dramatically within these ranges, from a mixture of nucleons, nuclei, and electrons to uniform, strongly interacting matter containing nucleons, and possibly other particles such as hyperons or quarks. As the development of an EoS requires joint efforts from many directions, different theoretical approaches are considered and relevant experimental and observational constraints which provide insights for future research are discussed. Finally, results from applications of the discussed EoS models are summarized.

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“…Actually there is a variety of neutron star properties which are sensitive to SE, that is the maximum mass value and the corresponding radius, the onset of the direct Urca process, the crust-core transition density and pressure e.t.c. [2,9] Recently, there is an extended theoretical [10,11,12,13,14,15,16,17,18,19,20,21,22,23,24,25,26,27,28,29,30,31,32,33,34,57,36,37,38,39,40,41,42,43,44,45,46,47,48,49,50,51,52,53,54,55,56,…”

Section: Introductionmentioning

confidence: 99%

Effects of the symmetry energy on the isovector properties of neutron-rich nuclei within a Thomas-Fermi approach

Papazoglou

Moustakidis

2014

Phys. Rev. C

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We employ a variational method, in the framework of the Thomas-Fermi approximation, to study the effect of the symmetry energy on the neutron skin thickness and the symmetry energy coefficients of various neutron rich nuclei. We concentrate our interest on 208 Pb, 124 Sn, 90 Zr, and 48 Ca, although the method can be applied in the totality of medium and heavy neutron rich nuclei. Our approach has the advantage that the isospin asymmetry function α(r), which is the key quantity to calculate isovector properties of various nuclei, is directly related with the symmetry energy as a consequence of the variational principle. Moreover, the Coulomb interaction is included in a self-consistent way and its effects can be separated easily from the nucleon-nucleon interaction. We confirm, both qualitatively and quantitatively, the strong dependence of the symmetry energy on the various isovector properties for the relevant nuclei, using possible constraints between the slope and the value of the symmetry energy at the saturation density. PACS number(s): 21.65. Ef, 21.65.Mn, 21.65.Cd, 21.10.Gv

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Density dependence of the nuclear symmetry energy from measurements of neutron radii in nuclei

Cited by 5 publications

References 89 publications

Effects of the liquid-gas phase transition and cluster formation on the symmetry energy

Effects of the liquid-gas phase transition and cluster formation on the symmetry energy

Equations of state for supernovae and compact stars

Effects of the symmetry energy on the isovector properties of neutron-rich nuclei within a Thomas-Fermi approach

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