Can the equation of state of asymmetric nuclear matter be studied using unstable nuclei?

Oyamatsu, Kazuhiro; Tanihata, I.; Sugahara, Yuichi; Sumiyoshi, Kohsuke; Toki, H.

doi:10.1016/s0375-9474(98)00125-0

Cited by 76 publications

(85 citation statements)

References 21 publications

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“…The labels A-I denote the sets for which we perform detailed calculations of the ground-state properties of inhomogeneous nuclear matter at subnuclear densities. For comparison, the values calculated from two mean-field models [TM1 (square) and SIII (dot)], which are known to be extreme cases [28], are plotted. The plot shows that our sets of (L, K 0 ) effectively cover such extreme cases.…”

Section: Model For Matter At Subnuclear Densitiesmentioning

confidence: 99%

Symmetry energy at subnuclear densities and nuclei in neutron star crusts

2007

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We examine how the properties of inhomogeneous nuclear matter at subnuclear densities depend on the density dependence of the symmetry energy. Using a macroscopic nuclear model we calculate the size and shape of nuclei in neutron star matter at zero temperature in a way dependent on the density dependence of the symmetry energy. We find that for smaller symmetry energy at subnuclear densities, corresponding to the larger density symmetry coefficient L, the charge number of nuclei is smaller and the critical density at which matter with nuclei or bubbles becomes uniform is lower. The decrease in the charge number is associated with the dependence of the surface tension on the nuclear density and the density of a sea of neutrons, whereas the decrease in the critical density can be generally understood in terms of proton clustering instability in uniform matter.

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Section: Model For Matter At Subnuclear Densitiesmentioning

confidence: 99%

Symmetry energy at subnuclear densities and nuclei in neutron star crusts

2007

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“…In the following, we construct the Wigner phase-space densities for deuteron, triton, and 3 He. The method can be generalized, although more involved, to the Wigner phase-space density for four-nucleon clusters (e.g., 4 He) and M -nucleon clusters.…”

Section: A the Coalescence Modelmentioning

confidence: 99%

“…Studies based on various theoretical models also give widely different predictions [3]. Lack of this knowledge has hampered our understanding of both the structure of radioactive nuclei [4,5,6,7] and many important issues in nuclear astrophysics [8,9,10], such as the nucleosynthesis during the pre-supernova evolution of massive stars and the properties of neutron stars [8,10]. However, recent advances in radioactive nuclear beam facilities provides a unique opportunity to study the density dependence of nuclear symmetry energy [3,11,12,13].…”

Section: Introductionmentioning

confidence: 99%

Light cluster production in intermediate energy heavy-ion collisions induced by neutron-rich nuclei

Chen¹,

Ko²,

Li³

2003

Nuclear Physics A

137

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The coalescence model based on nucleon distribution functions from an isospin-dependent transport model is used to study the production of deuteron, triton, and 3 He from heavy-ion collisions induced by neutron-rich nuclei at intermediate energies. It is found that the emission time of these light clusters depends on their masses. For clusters with same momentum per nucleon, heavier ones are emitted earlier. Both the yield and energy spectrum of light clusters are sensitive to the density dependence of nuclear symmetry energy, with more light clusters produced in the case of a stiff symmetry energy. On the other hand, effects due to the stiffness of the isoscalar part of nuclear equation of state and the medium dependence of nucleon-nucleon cross sections on light cluster production are unimportant. We have also studied the correlation functions of clusters, and they are affected by the density dependence of nuclear symmetry energy as well, with the stiff symmetry energy giving a stronger anti-correlation of light clusters, particularly for those with large kinetic energies. Dependence of light cluster production on the centrality and incident energy of heavy ion collisions as well as the mass of the reaction system is also investigated.

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“…In particular it has been shown by Tanihata [13] that in shf the saturation density essentially does not change, but in rmf it decreases rapidly as nuclear matter becomes more neutronrich. Most eos used in the description of neutron stars and supernova are obtained from nonrelativistic models.…”

Section: Introductionmentioning

confidence: 97%

“…The authors of references [13] and [14] have recently stressed the possibility of extracting the eos of asymmetric nuclear matter through the investigation of these properties as well as via reactions of neutron-rich nuclei at intermediate energies.…”

Section: Introductionmentioning

confidence: 99%