Nucleon-nucleon cross sections in dense nuclear matter

Zhang, H. F.; Li, Z. H.; Lombardo, U.; Luo, Peng; Sammarruca, Francesca; Zuo, Wei

doi:10.1103/physrevc.76.054001

Cited by 56 publications

(80 citation statements)

References 29 publications

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“…It should vary from m * n ≈ 0.6 m n at ρ ∼ 1.5 × 10 14 g cm −3 to 0.45 m n at ρ ∼ 6 × 10 14 g cm −3 . Let us note, that the inclusion of three-nucleon interactions does reduce m * n , and the reduction increases with density [12]. However, since we do not know exact values of m * n , used in Ref.…”

Section: A Equations Of Statementioning

confidence: 99%

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Shear viscosity in neutron star cores

Shternin¹,

Yakovlev²

2008

Phys. Rev. D

120

264

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We calculate the shear viscosity η ≈ ηeµ +ηn in a neutron star core composed of nucleons, electrons and muons (ηeµ being the electron-muon viscosity, mediated by collisions of electrons and muons with charged particles, and ηn the neutron viscosity, mediated by neutron-neutron and neutronproton collisions). Deriving ηeµ, we take into account the Landau damping in collisions of electrons and muons with charged particles via the exchange of transverse plasmons. It lowers ηeµ and leads to the non-standard temperature behavior ηeµ ∝ T −5/3 . The viscosity ηn is calculated taking into account that in-medium effects modify nucleon effective masses in dense matter. Both viscosities, ηeµ and ηn, can be important, and both are calculated including the effects of proton superfluidity. They are presented in the form valid for any equation of state of nucleon dense matter. We analyze the density and temperature dependence of η for different equations of state in neutron star cores, and compare η with the bulk viscosity in the core and with the shear viscosity in the crust.

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Section: A Equations Of Statementioning

confidence: 99%

“…Our approach is similar to that used by Baiko, Haensel and Yakovlev [11] (hereafter BHY01) for evaluating the thermal conductivity of neutrons. In addition, we employ recent developments [12] in calculations of nucleon-nucleon scattering cross sections in nuclear matter. As in BHY01, we take into account superfluidity of protons.…”

Section: Introductionmentioning

confidence: 99%

Shear viscosity in neutron star cores

Shternin¹,

Yakovlev²

2008

Phys. Rev. D

120

264

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“…[87,93,[395][396][397][398][399][400][401][402][403][404][405][406][407][408][409][410][411]. Most of theses studies are carried out for symmetric nuclear matter at zero temperature, and the results vary considerably.…”

Section: Theoretical Predictions and Experimental Information On Nn Cmentioning

confidence: 99%

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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“…Besides improving the framework of transport model from semi-classical transport to quantum transport [75], it would be nice to make thorough studies on the scattering cross sections, especially, of isospin-dependent nucleon-nucleon in medium [76][77][78] and symmetry potential of nucleon in asymmetric matter [79]. And also some unknown nucleon-nucleon interaction such as the tensor force induced isospin-dependence of short-range nucleonnucleon correlation [80] and spin-orbit potential [81] may also affect isospin sensitive observables in heavy-ion collisions.…”

Section: Conclusion and Remarksmentioning

confidence: 99%

Model dependence of isospin sensitive observables at high densities

et al. 2013

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Within two different frameworks of isospin-dependent transport model, i.e., Boltzmann-UehlingUhlenbeck (IBUU04) and Ultrarelativistic Quantum Molecular Dynamics (UrQMD) transport models, sensitive probes of nuclear symmetry energy are simulated and compared. It is shown that neutron to proton ratio of free nucleons, π − /π + ratio as well as isospin-sensitive transverse and elliptic flows given by the two transport models with their "best settings", all have obvious differences. Discrepancy of numerical value of isospin-sensitive n/p ratio of free nucleon from the two models mainly originates from different symmetry potentials used and discrepancies of numerical value of charged π − /π + ratio and isospin-sensitive flows mainly originate from different isospin-dependent nucleon-nucleon cross sections. These demonstrations call for more detailed studies on the model inputs (i.e., the density-and momentum-dependent symmetry potential and the isospin-dependent nucleon-nucleon cross section in medium) of isospin-dependent transport model used. The studies of model dependence of isospin sensitive observables can help nuclear physicists to pin down the density dependence of nuclear symmetry energy through comparison between experiments and theoretical simulations scientifically.

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Nucleon-nucleon cross sections in dense nuclear matter

Cited by 56 publications

References 29 publications

Shear viscosity in neutron star cores

Shear viscosity in neutron star cores

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

Model dependence of isospin sensitive observables at high densities

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