Bao_An_Li.ppt.pptVIP

Constraining the radii of NON-ROTATING neutron stars APR: K0=269 MeV. The same incompressibility for symmetric nuclear matter of K0=211 MeV for x=0, -1, and -2 Bao-An Li and Andrew W. Steiner, Phys. Lett. B642, 436 (2006) Nuclear limits ● . * * * * * * * * * * * * * * Probing the symmetry energy at high densities Outline: Why is the symmetry energy so uncertain at supra-saturation densities? Can the symmetry energy become super-soft or even negative at high densities? --- Some observations by a non-expert of many-body theories Indications of a super-soft symmetry energy at supra-saturation densities from transport model analyses of the FOPI/GSI experimental data on pion production Can neutron stars be stable with a super-soft or negative symmetry energy at supra-saturation densities? --- Some observations and attempts by a non-expert of astrophysics collaborators: De-Hua Wen and Chang Xu, Texas AM University-Commerce Lie-Wen Chen, Shanghai Jiao-Tung University Zhigang Xiao and Ming Zhang, Tsinghua University, China Gao-Chan Yong, Institute of Modern Physics, China Bao-An Li Esym (ρ) predicted by microscopic many-body theories Symmetry energy (MeV) Density Effective field theory DBHF RMF BHF Greens function Variational A.E. L. Dieperink et al., Phys. Rev. C68 (2003) 064307 Why is the symmetry energy so uncertain especially at high densities?Based on the Fermi gas model (Ch. 6) and properties of nuclear matter (Ch. 8) of the textbook: Structure of the nucleus by M.A. Preston and R.K. Bhaduri Kinetic Isoscalar Isovector Correlation function Nuclear Structure based on Correlated Realistic Nucleon-Nucleon Potentials R. Roth, T. Neff, H. Hergert, H. Feldmeier, Nucl. Phys. A745 (2004) 3-33 Tensor correlations in the Unitary Correlation Operator Method Thomas Neff, Hans Feldmeier, Nucl. Phys. A713 (2003) 311-371 Correlation function At saturation density Using Paris potential I. Bombaci and U. Lombardo PRC 44, 1892 (1991) Using the Reid