Bulletin of the American Physical Society
6th Joint Meeting of the APS Division of Nuclear Physics and the Physical Society of Japan
Sunday–Friday, November 26–December 1 2023; Hawaii, the Big Island
Session 4WLB: Equation of State of Dense Nuclear Matter IIInvited Workshop
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Chair: Bao-An Li, Texas A&M University–Commerce Room: Hilton Waikoloa Village Kona 5 |
Monday, November 27, 2023 4:00PM - 4:30PM |
4WLB.00001: EOS from exapanding and clusterizing matter in heavy-ion collisions Invited Speaker: Akira Ono In heavy-ion collisions at several hundred MeV/nucleon, a compressed nuclear system is formed up to about twice the saturation density and then rapidly expands. It has been a theoretical challenge to extract information on nuclear matter properties such as the EOS of isospin-asymmetric nuclear matter. Even though one may be tempted to regard the global collision evolution as one-body dynamics in phase space, light clusters and heavier fragment nuclei are copiously produced and measured in experiments. The many-body correlations to form them can be so strong that they affect the global collision evolution. |
Monday, November 27, 2023 4:30PM - 5:00PM |
4WLB.00002: Experimental study of asymmetric nuclear matter EoS from heavy-ion reactions Invited Speaker: Tadaaki Isobe Neutron star (NS) is believed to be created as a remnant of supernova explosion. The property of neutron star can be described with the thermodynamical character (Equation of State, EoS) of nuclear matter. For the determination of outer core NS-EoS, we have performed a series of measurements using heavy ion accelerator experimental facilities in Japan, such as RIKEN Radio Isotope Beam Factory (RIBF) and Heavy Ion Medical Accelerator in Chiba. |
Monday, November 27, 2023 5:00PM - 5:30PM |
4WLB.00003: Probing Symmetry Energy of Dense Neutron-Rich Matter Invited Speaker: Bao-An Li Neutron-rich matter exists naturally in neutron stars and some nuclei. It can also be created during mergers of neutron stars in space and collisions between two heavy nuclei in terrestrial nuclear laboratories. The nature and Equation of State (EOS) of such matter are still very poorly known while they have broad impacts on many interesting issues in both astrophysics and nuclear physics. In particular, nuclear symmetry energy encoding the energy cost to make 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 as the strain amplitude and frequencies of gravitational waves from neutron star mergers. |
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