2005
DOI: 10.1016/j.nuclphysa.2005.03.002
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Momentum and density dependence of the isospin part of nuclear mean field and equation of state of asymmetric nuclear matter

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Cited by 39 publications
(61 citation statements)
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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%
“…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%
“…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%
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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%