Topic（题目）：Probing the Equation of State of Dense Neutron-Rich Matter with Terrestrial Experiments and Astrophysical Observations
Speaker（报告人）：Bao-An Li (Texas A&M University-Commerce)
Neutron-rich matter exists naturally in neutron stars and neutron skins of heavy nuclei. It can also be created during mergers of neutron stars in space and heavy-ion collisions in terrestrial laboratories. The Equation of State (EOS) of such matter is still very poorly known but has broad impacts on many interesting issues in both astrophysics and nuclear physics. In particular, nuclear symmetry energy encoding the energy cost to make the nuclear matter more neutron-rich has been the most uncertain part of the EOS of dense neutron-rich nucleonic matter. It affects the masses, radii, tidal deformations, cooling rates, and frequencies of various oscillation modes of isolated neutron stars as well asthestrain amplitude and frequencies of gravitational waves from neutron star mergers.
In this talk, we will discuss several key issues and some recent progress in constraining the EOS of dense neutron-rich matter, especially the density dependence of nuclear symmetry energy.
Prof. Bao-An Li received his Ph.D. degree from Michigan State University in 1992 and was elected a Fellow of the American Physical Society in 2013 “forhis important contributions to our understanding of asymmetric nuclear matter and for his untiring efforts in promoting isospin physics worldwide”. He is currentlya Texas A&M University System Regents’ Professor working on the Commerce campus. Before and after receiving his Ph.D degree, he worked in various positions at the Institute of Modern Physics in Lanzhou, Oak Ridge National Laboratory, Niels Bohr Institute, Hahn-Meitner Institute, Texas A&M University and Arkansas State University before joining the Texas A&M University-Commerce in 2006 as the Head of its Department of Physics and Astronomy for 5 years. His research interests are in understanding the dynamics of nuclear reactions from low to ultra-relativistic energies, the Equation of State of neutron-rich nuclear matter as well as its impacts on properties of nuclei, nuclear reactions, neutron stars and gravitational waves.