Momentum and density dependence of the isospin part of nuclear mean field and equation of state of asymmetric nuclear matter

Behera, Banarji; Routray, T. R.; Pradhan, A.; Patra, S. K.; Sahu, P. K.

doi:10.1016/j.nuclphysa.2005.03.002

Cited by 38 publications

(60 citation statements)

References 63 publications

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“…It is to note here that the values of the functional E N SM asy (ρ, Y p ) corresponding to the universal behaviour obtained as a function of density in the cases of the EOSs constructed from relativistic and non-relativistic considerations in Refs. [32] and [33], respectively, are in close agreement with the model independent values found in this work. In this context it can be mentioned here that although recent observations of neutron star cooling [24][25][26][27][28][29] suggest that fast cooling through DU processes should not occur in neutron stars and the universal high density behaviour of the functional E N SM asy (ρ, Y p ) leads to a density dependence of V s (ρ) in consistent with these observations.…”

Section: Introductionsupporting

confidence: 91%

Density dependence of nuclear symmetry energy

2016

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High density behaviour of nuclear symmetry energy is studied on the basis of a stiffest density dependence of asymmetric contribution to energy per nucleon in charge neutral n + p + e + µ matter under beta equilibrium. The density dependence of nuclear symmetry energy obtained in this way is neither very stiff nor soft at high densities and is found to be in conformity with recent observations of neutron stars PACS: 21.65.+f; 26.60.+c

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Section: Introductionsupporting

confidence: 91%

Density dependence of nuclear symmetry energy

2016

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“…As discussed above, microscopic many-body theories, such as the relativistic DBHF [101][102][103]235,236] and nonrelativistic BHF approaches [88,89,274,286], predict that m * n > m * p in neutron-rich matter. On the other hand, opposite results are predicted by some effective interactions within phenomenological approaches including the SHF and potential models as well as all RMF models [50,211,233]. As an example, shown in Fig.…”

Section: Microscopic Approachesmentioning

confidence: 84%

“…Recently, there is a renewed interest in the isovector part of the nucleon mean-field potential, i.e., the nuclear symmetry potential, in isospin asymmetric nuclear matter [6,48,50,51,71,88,[101][102][103]210,[231][232][233][234][235][236][237][238][239][240]. As discussed in Chapter 1 and other Chapters of this review, knowledge on the symmetry potential is important for understanding not only the structure and reactions of radioactive nuclei but also many critical issues in astrophysics.…”

Section: The Momentum Dependence Of the Isovector Potential And The Nmentioning

confidence: 99%

“…Besides depending on the nuclear density, the symmetry potential also depends on the momentum or energy of a nucleon. The various microscopic and phenomenological approaches, such as the relativistic DBHF [101][102][103]231,235,239] and the non-relativistic BHF [88,234] approach, the chiral perturbation theory [141], the RMF approach [6,211], and the non-relativistic mean-field theory based on Skyrmelike interactions [210,232,233,241], that are described in Chapter 2 for studying the symmetry energy and potential, as well as the relativistic impulse approximation [238,240] all give widely different predictions for the momentum dependence of the nuclear symmetry potential, as in their predictions for the density dependence of the nuclear symmetry energy. For example, while most models predict a decreasing symmetry potential with increasing nucleon momentum albeit at different rates, a few nuclear effective interactions used in some of the models lead to an opposite conclusion.…”

Section: The Momentum Dependence Of the Isovector Potential And The Nmentioning

confidence: 99%

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Recent progress and new challenges in isospin physics with heavy-ion reactions

2008

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The ultimate goal of studying isospin physics via heavy-ion reactions with neutron-rich, stable and/or radioactive nuclei is to explore the isospin dependence of in-medium nuclear effective interactions and the equation of state of neutron-rich nuclear matter, particularly the isospin-dependent term in the equation of state, i.e., the density dependence of the symmetry energy. Because of its great importance for understanding many phenomena in both nuclear physics and astrophysics, the study of the density dependence of the nuclear symmetry energy has been the main focus of the intermediate-energy heavy-ion physics community during the last decade, and significant progress has been achieved both experimentally and theoretically. In particular, a number of phenomena or observables have been identified as sensitive probes to the density dependence of the nuclear symmetry energy. Experimental studies have confirmed some of these interesting isospin-dependent effects and allowed us to constrain relatively stringently the symmetry energy at sub-saturation densities. The impacts of this constrained density dependence of the symmetry energy on the properties of neutron stars have also been studied, and they were found to be very useful for the astrophysical community. With new opportunities provided by the various radioactive beam facilities being constructed around the world, the study of isospin physics is expected to remain one of the forefront research areas in nuclear physics. In this report, we review the major progress achieved during the last decade in isospin physics with heavy ion reactions and discuss future challenges to the most important issues in this field.Key words: Equation of state of asymmetric nuclear matter, Nuclear symmetry energy, Heavy-ion reactions with neutron-rich nuclei, Neutron skin thickness of heavy nuclei, Neutron stars Constraining the Skyrme effective interactions and the neutron skin thickness of heavy nuclei using terrestrial nuclear laboratory data 216 8

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“…Although the nuclear symmetry energy at ρ 0 is known to be around 30 MeV from the empirical liquid-drop mass formula [27,28], its values at other densities, especially at supra-saturation densities, are poorly known [6,7]. Various microscopic and phenomenological models, such as the relativistic Dirac-Brueckner-HartreeFock (DBHF) [29][30][31][32][33][34][35] and the nonrelativistic BruecknerHartree-Fock (BHF) [36][37][38][39] approach, the relativistic mean-field (RMF) model based on nucleon-meson interactions [12,[40][41][42], and the nonrelativistic mean-field model based on Skyrme-like interactions [43][44][45][46][47][48][49][50][51], have been used to study the isospin-dependent properties of asymmetric nuclear matter, such as the nuclear symmetry energy, the nuclear symmetry potential, and the isospin-splitting of the nucleon effective masses, but the predicted results vary widely. In fact, even the sign of the symmetry energy above 3ρ 0 is still uncertain [52,53].…”

Section: Introductionmentioning

confidence: 99%

Higher-order effects on the incompressibility of isospin asymmetric nuclear matter

et al. 2009

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Analytical expressions for the saturation density of asymmetric nuclear matter as well as its binding energy and incompressibility at saturation density are given up to fourth order in the isospin asymmetry δ = (ρ n − ρ p )/ρ using 11 characteristic parameters defined by the density derivatives of the binding energy per nucleon of symmetric nuclear matter, the symmetry energy E sym (ρ), and the fourth-order symmetry energy E sym,4 (ρ) at normal nuclear density ρ 0 . Using an isospin-and momentum-dependent modified Gogny interaction (MDI) and the Skyrme-Hartree-Fock (SHF) approach with 63 popular Skyrme interactions, we have systematically studied the isospin dependence of the saturation properties of asymmetric nuclear matter, particularly the incompressibilityat saturation density. Our results show that the magnitude of the higher order K sat,4 parameter is generally small compared to that of the K sat,2 parameter. The latter essentially characterizes the isospin dependence of the incompressibility at saturation density and can be expressed asL, where L and K sym represent, respectively, the slope and curvature parameters of the symmetry energy at ρ 0 and J 0 is the third-order derivative parameter of symmetric nuclear matter at ρ 0 . Furthermore, we have constructed a phenomenological modified Skyrme-like (MSL) model that can reasonably describe the general properties of symmetric nuclear matter and the symmetry energy predicted by both the MDI model and the SHF approach. The results indicate that the higher order J 0 contribution to K sat,2 generally cannot be neglected. In addition, it is found that there exists a nicely linear correlation between K sym and L as well as between J 0 /K 0 and K 0 . These correlations together with the empirical constraints on K 0 , L, E sym (ρ 0 ), and the nucleon effective mass lead to an estimate of K sat,2 = −370 ± 120 MeV.

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Momentum and density dependence of the isospin part of nuclear mean field and equation of state of asymmetric nuclear matter

Cited by 38 publications

References 63 publications

Density dependence of nuclear symmetry energy

Density dependence of nuclear symmetry energy

Recent progress and new challenges in isospin physics with heavy-ion reactions

Higher-order effects on the incompressibility of isospin asymmetric nuclear matter

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