Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars

Providência, Constança; Avancini, S. S.; Cavagnoli, Rafael; Chiacchiera, Silvia; Ducoin, C.; Grill, Fabrizio; Margueron, J.; Menezes, D. P.; Rabhi, Aziz; Vidaña, Isaac

doi:10.1140/epja/i2014-14044-7

Cited by 52 publications

(32 citation statements)

References 102 publications

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“…Note that the interplay between L and the hyperon content of neutron stars has been studied in detail in Refs. [31][32][33]. Our results are compatible with those studies.…”

Section: Resultssupporting

confidence: 93%

Early appearance ofΔisobars in neutron stars

et al. 2014

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We discuss the formation of isobars in neutron star matter. We show that their threshold density strictly correlates with the density derivative of the symmetry energy of nuclear matter: the L parameter. By restricting L to the range of values indicated by recent experimental and theoretical analysis, i.e., 40 MeV L 62 MeV, we find that isobars appear at a density of the order of 2 to 3 times the nuclear matter saturation density, i.e., the same range as for the appearance of hyperons. The range of values of the couplings of the s with the mesons is restricted by the analysis of the data obtained from photoabsorption, electron and pion scattering on nuclei. If the potential of the in nuclear matter is close to the one indicated by the experimental data then the equation of state becomes soft enough that a " puzzle" exists, similar to the "hyperon puzzle" widely discussed in the literature. Possible solutions to this puzzle are also discussed.

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“…Note that the interplay between L and the hyperon content of neutron stars has been studied in detail in Refs. [31][32][33]. Our results are compatible with those studies.…”

Section: Resultssupporting

confidence: 93%

Early appearance ofΔisobars in neutron stars

et al. 2014

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“…The proton and neutron effective masses, M * p and M * n , and the scalar potential are also defined as in Eqs. (20) and (19), respectively, observing the generalizations in Eq. (26).…”

Section: Relativistic Mean-field Models At Zero Temperaturementioning

confidence: 99%

“…[18,19] and a comprehensive study of the imprint of the symmetry energy on the crust and strangeness content of neutron star can be seen in Ref. [20]. Moreover, in Refs.…”

Section: Introductionmentioning

confidence: 98%

Relativistic mean-field hadronic models under nuclear matter constraints

et al. 2014

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Background:The microscopic composition and properties of infinite hadronic matter at a wide range of densities and temperatures have been subjects of intense investigation for decades. The equation of state (EoS) relating pressure, energy density, and temperature at a given particle number density is essential for modeling compact astrophysical objects such as neutron stars, core-collapse supernovae, and related phenomena, including the creation of chemical elements in the universe. The EoS depends not only on the particles present in the matter, but, more importantly, also on the forces acting among them. Because a realistic and quantitative description of infinite hadronic matter and nuclei from first principles in not available at present, a large variety of phenomenological models has been developed in the past several decades, but the scarcity of experimental and observational data does not allow a unique determination of the adjustable parameters. Purpose: It is essential for further development of the field to determine the most realistic parameter sets and to use them consistently. Recently, a set of constraints on properties of nuclear matter was formed and the performance of 240 nonrelativistic Skyrme parametrizations was assessed [M. Dutra et al., Phys. Rev. C 85, 035201 (2012)] in describing nuclear matter up to about three times nuclear saturation density. In the present work we examine 263 relativistic-mean-field (RMF) models in a comparable approach. These models have been widely used because of several important aspects not always present in nonrelativistic models, such as intrinsic Lorentz covariance, automatic inclusion of spin, appropriate saturation mechanism for nuclear matter, causality, and, therefore, no problems related to superluminal speed of sound in medium. Method: Three different sets of constraints related to symmetric nuclear matter, pure neutron matter, symmetry energy, and its derivatives were used. The first set (SET1) was the same as used in assessing the Skyrme parametrizations. The second and third sets (SET2a and SET2b) were more suitable for analysis of RMF and included, up-to-date theoretical, experimental and empirical information. Results: The sets of updated constraints (SET2a and SET2b) differed somewhat in the level of restriction but still yielded only 4 and 3 approved RMF models, respectively. A similarly small number of approved Skyrme parametrizations were found in the previous study with Skyrme models. An interesting feature of our analysis 0556-2813/2014/90(5)/055203 (35) 055203-1 ©2014 American Physical Society M. DUTRA et al.PHYSICAL REVIEW C 90, 055203 (2014) has been that the results change dramatically if the constraint on the volume part of the isospin incompressibility (K τ,v ) is eliminated. In this case, we have 35 approved models in SET2a and 30 in SET2b. Conclusions: Our work provides a new insight into application of RMF models to properties of nuclear matter and brings into focus their problematic proliferation. The assessment performed in this wo...

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“…However, J and L 0 can be easily controlled by the inclusion of a ωρ interaction, as discussed in Refs. [31][32][33]. As the value of this interaction gets larger, the the values of the symmetry energy and its slope become lower.…”

Section: The Quark-meson Coupling Modelmentioning

confidence: 99%

Nuclear pasta phases within the quark-meson coupling model

et al. 2017

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In this work, the low-density regions of nuclear and neutron star matter are studied. The search for the existence of nuclear pasta phases in this region is performed within the context of the quark-meson coupling (QMC) model, which incorporates quark degrees of freedom. Fixed proton fractions are considered, as well as nuclear matter in β equilibrium at zero temperature. We discuss the recent attempts to better understand the surface energy in the coexistence phases regime and we present results that show the existence of the pasta phases subject to some choices of the surface energy coefficient. We also analyze the influence of the nuclear pasta on some neutron star properties. The equation of state containing the pasta phase will be part of a complete grid for future use in supernova simulations.

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Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars

Cited by 52 publications

References 102 publications

Early appearance ofΔisobars in neutron stars

Early appearance ofΔisobars in neutron stars

Relativistic mean-field hadronic models under nuclear matter constraints

Nuclear pasta phases within the quark-meson coupling model

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