Extracting the equation of state(EOS) and symmetry energy of dense neutron-rich matter from astrophysical observations is a long-standing goal of nuclear astrophysics. To facilitate the realization of this goal, the f...Extracting the equation of state(EOS) and symmetry energy of dense neutron-rich matter from astrophysical observations is a long-standing goal of nuclear astrophysics. To facilitate the realization of this goal, the feasibility of using an explicitly isospin-dependent parametric EOS for neutron star matter was investigated recently in [1–3]. In this contribution, in addition to outlining the model framework and summarizing the most important findings from [1–3], we report a few new results regarding constraining parameters characterizing the highdensity behavior of nuclear symmetry energy. In particular,the constraints on the pressure of neutron star matter extracted from combining the X-ray observations of the neutron star radius, the minimum–maximum mass M=2:01 M_⊙, and causality condition agree very well with those extracted from analyzing the tidal deformability data by the LIGO ? Virgo Collaborations. The limitations of using the radius and/or tidal deformability of neutron stars to constrain the high-density nuclear symmetry energy are discussed.展开更多
We examine critically how tightly the density dependence of nuclear symmetry energy E_(sym)(q) is constrained by the universal equation of state of the unitary Fermi gas EUG(q) considering currently known uncertaintie...We examine critically how tightly the density dependence of nuclear symmetry energy E_(sym)(q) is constrained by the universal equation of state of the unitary Fermi gas EUG(q) considering currently known uncertainties of higher order parameters describing the density dependence of the equation of state of isospin asymmetric nuclear matter. We found that E_(UG)(q) does provide a useful lower boundary for the E_(sym)(q). However, it doesnot tightly constrain the correlation between the magnitude E_(sym)(q_0) and slope L unless the curvature K_(sym)of the symmetry energy at saturation density q_0 is more precisely known. The large uncertainty in the skewness parameters affects the E_(sym)(q_0) versus L correlation by the same almost as significantly as the uncertainty in K_(sym).展开更多
In this talk,we first briefly review the isospin dependence of the total nucleon effective mass M Jinferred from analyzing nucleon-nucleus scattering data within an isospin-dependent non-relativistic optical potential...In this talk,we first briefly review the isospin dependence of the total nucleon effective mass M Jinferred from analyzing nucleon-nucleus scattering data within an isospin-dependent non-relativistic optical potential model,and the isospin dependence of the nucleon E-mass M;E J obtained from applying the Migdal–Luttinger theorem to a phenomenological single-nucleon momentum distribution in nuclei constrained by recent electron-nucleus scatteringexperiments.Combining information about the isospin dependence of both the nucleon total effective mass and E-mass,we then infer the isospin dependence of nucleon k-mass using the well-known relation M_J~*=M_ J^(*1E).Implications of the results on the nucleon mean free path in neutron-rich matter are discussed.展开更多
Nuclear clusters or voids in the inner crust of neutron stars were predicted to have various shapes collectively nicknamed nuclear pasta.The recent review in Ref.[1]by Lopez,Dorso and Frank summarized their systematic...Nuclear clusters or voids in the inner crust of neutron stars were predicted to have various shapes collectively nicknamed nuclear pasta.The recent review in Ref.[1]by Lopez,Dorso and Frank summarized their systematic investigations into properties especially the mor-phological and thermodynamical phase transitions of the nuclear pasta within a Classical Molecular Dynamics model,providing further stimuli to find more observational evidences of the predicted nuclear pasta in neutron stars.展开更多
基金NBZ was supported in part by the China Scholarship Councilthe U.S.Department of Energy,Office of Science,under Award Number DE-SC0013702,the CUSTIPEN(China-U.S.Theory Institute for Physics with Exotic Nuclei)under the U.S.Department of Energy Grant No.DE-SC0009971the National Natural Science Foundation of China under Grant No.11320101004
文摘Extracting the equation of state(EOS) and symmetry energy of dense neutron-rich matter from astrophysical observations is a long-standing goal of nuclear astrophysics. To facilitate the realization of this goal, the feasibility of using an explicitly isospin-dependent parametric EOS for neutron star matter was investigated recently in [1–3]. In this contribution, in addition to outlining the model framework and summarizing the most important findings from [1–3], we report a few new results regarding constraining parameters characterizing the highdensity behavior of nuclear symmetry energy. In particular,the constraints on the pressure of neutron star matter extracted from combining the X-ray observations of the neutron star radius, the minimum–maximum mass M=2:01 M_⊙, and causality condition agree very well with those extracted from analyzing the tidal deformability data by the LIGO ? Virgo Collaborations. The limitations of using the radius and/or tidal deformability of neutron stars to constrain the high-density nuclear symmetry energy are discussed.
基金supported in part by the China Scholarship Councilthe U.S.Department of Energy,Office of Science,under Award Number DE-SC0013702+7 种基金the CUSTIPEN(China-U.S.Theory Institute for Physics with Exotic Nuclei) under the US Department of Energy Grant No.DE-SC0009971the National Natural Science Foundation of China under Grant No.11320101004the Texas Advanced Computing Centersupported in part by the Major State Basic Research Development Program(973Program) of China under Contract Nos.2015CB856904 and 2014CB845401the National Natural Science Foundation of China under Grant Nos.11475243 and 11421505the ‘‘100-talent plan’’ of Shanghai Institute of Applied Physics under Grant Nos.Y290061011and Y526011011 from the Chinese Academy of Sciencesthe Shanghai Key Laboratory of Particle Physics and Cosmology under Grant No.15DZ2272100the Shanghai Pujiang Program under Grant No.13PJ1410600
文摘We examine critically how tightly the density dependence of nuclear symmetry energy E_(sym)(q) is constrained by the universal equation of state of the unitary Fermi gas EUG(q) considering currently known uncertainties of higher order parameters describing the density dependence of the equation of state of isospin asymmetric nuclear matter. We found that E_(UG)(q) does provide a useful lower boundary for the E_(sym)(q). However, it doesnot tightly constrain the correlation between the magnitude E_(sym)(q_0) and slope L unless the curvature K_(sym)of the symmetry energy at saturation density q_0 is more precisely known. The large uncertainty in the skewness parameters affects the E_(sym)(q_0) versus L correlation by the same almost as significantly as the uncertainty in K_(sym).
基金supported in part by the US Department of Energy’s Office of Science under Award Number DE-SC0013702the CUSTIPEN(China-US Theory Institute for Physics with Exotic Nuclei)under the US Department of Energy Grant No.DESC0009971+6 种基金the National Natural Science Foundation of China Under Grant Nos.11320101004,11275125,11205083 and 11135011the Major State Basic Research Development Program(973 Program)in China under Contract Nos.2013CB834405 and 2015CB856904the‘‘Shu Guang’’project supported by Shanghai Municipal Education Commission and Shanghai Education Development Foundationthe Program for Professor of Special Appointment(Eastern Scholar)at Shanghai Institutions of Higher Learning,the Science and Technology Commission of Shanghai Municipality(11DZ2260700)the construct program of the key discipline in Hunan province,the Research Foundation of Education Bureau of Hunan Province,China(Grant No.15A159)the Natural Science Foundation of Hunan Province,China(Grant No.2015JJ3103)the Innovation Group of Nuclear and Particle Physics in USC
文摘In this talk,we first briefly review the isospin dependence of the total nucleon effective mass M Jinferred from analyzing nucleon-nucleus scattering data within an isospin-dependent non-relativistic optical potential model,and the isospin dependence of the nucleon E-mass M;E J obtained from applying the Migdal–Luttinger theorem to a phenomenological single-nucleon momentum distribution in nuclei constrained by recent electron-nucleus scatteringexperiments.Combining information about the isospin dependence of both the nucleon total effective mass and E-mass,we then infer the isospin dependence of nucleon k-mass using the well-known relation M_J~*=M_ J^(*1E).Implications of the results on the nucleon mean free path in neutron-rich matter are discussed.
基金Acknowledgements This work was supported by the Major State Basic Research Development Program （973 Program） of China under Contract Nos. 2015CB856904 and 2014CB845401, the National Natural Science Foundation of China under Grant Nos. 11320101004, 11475243, and 11421505, the ＂100-Talent Plan＂ of Shanghai Institute of Applied Physics under Grant Nos. Y290061011 and Y526011011 from the Chinese Academy of Sciences, the ＂Shanghai Pujiang Program＂ under Grant No. 13PJ1410600, the U.S. National Science Foundation under Grant No. PHY-1068022, the U.S. Department of Energy Office of Science under Award No. DE-SC0013702, and the CUSTIPEN （China- U.S. Theory Institute for Physics with Exotic Nuclei） under the U.S. Department of Energy Grant No. DE-FG02-13ER42025.
基金B. A. Li is supported in part by the U.S.D epartm ent of Energy, Office of Science, under Award Number DESC0013702the CUSTIPEN (China-U.S. Theory Institute for Physics with Exotic Nuclei) under the US D epartment of Energy Grant No. DE-SC0009971.
文摘Nuclear clusters or voids in the inner crust of neutron stars were predicted to have various shapes collectively nicknamed nuclear pasta.The recent review in Ref.[1]by Lopez,Dorso and Frank summarized their systematic investigations into properties especially the mor-phological and thermodynamical phase transitions of the nuclear pasta within a Classical Molecular Dynamics model,providing further stimuli to find more observational evidences of the predicted nuclear pasta in neutron stars.
