Bulletin of the American Physical Society
2010 Fall Meeting of the APS Division of Nuclear Physics
Volume 55, Number 14
Tuesday–Saturday, November 2–6, 2010; Santa Fe, New Mexico
Session NB: Nuclear Symmetry Energy of the Nuclear Matter EOS |
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Chair: Bao-An Li, Texas A&M University - Commerce Room: Sweeny B |
Saturday, November 6, 2010 10:30AM - 11:06AM |
NB.00001: Recent Results and Experimentation Using Isotopic Obervables as Sensitive Parameters of the Asymmetry Term of the Nuclear Equation-of-State Invited Speaker: The characterization of the density dependence of the nuclear equation-of-state (EOS) remains a longstanding problem in nuclear astrophysics. While observations of neutron star masses have placed astronomical lower limits on the asymmetry term of the EOS, experimental constraints remain open. Recent improvements in experiment, data interpretation, and theoretical predictions have greatly reduced the constraints on what is known concerning this dependence. Future work must focus on studying the nuclear EOS at higher-density ($\rho>\rho_o$). Recent heavy-ion beam experimentation will be described, and the theoretical interpretation will be presented. Of particular importance are plans to increase the density of the explored region of the nuclear EOS. The applications of experimental results from $^{40,48}$Ca+$^{112,124}$Sn reactions at 140 MeV/A will also be covered. These reactions were studied to constrain the in-medium nucleon masses, which are a considerable unknown in model predictions of the nuclear EOS. Finally, applications of nuclear experimental results to neutron-star macroscopic structure will be presented. [Preview Abstract] |
Saturday, November 6, 2010 11:06AM - 11:42AM |
NB.00002: Bridging Nuclear Physics and Astrophysics with the Nuclear Symmetry Energy Invited Speaker: The nuclear symmetry energy, a critical input for nuclear structure, heavy-ion collisions, and several astrophysical processes, is the most uncertain aspect of the nucleon-nucleon interaction. In this talk, I describe how recent experiments and observations are constraining the symmetry energy and building bridges between terrestrial experiments and astronomical observations. From the observational side, neutron star cooling, mass and radius measurements, and oscillations in magnetar flares will be discussed. These astrophysical properties are connected, through the nuclear symmetry energy, to the structure of neutron-rich nuclei, intermediate-energy heavy-ion collisions, and the neutron skin thickness of lead. As a result of these connections, a clear preference for a softer symmetry energy and smaller neutron star radii will be demonstrated. Most importantly, I will show that future experiments and observations can quantitatively improve our understanding of the symmetry energy and thus the nucleon-nucleon interaction. [Preview Abstract] |
Saturday, November 6, 2010 11:42AM - 12:18PM |
NB.00003: Elucidating the Symmetry Energy of Nuclear Matter with Heavy-ion Reactions Invited Speaker: The equation of state (EOS) of nuclear matter is of fundamental importance to both nuclear physics and astrophysics. While there has been significant progress in understanding the EOS of symmetric nuclear matter, there is still considerable uncertainty in the EOS of asymmetric nuclear matter. Our understanding of the density dependence of the nuclear symmetry energy is limited. Understanding the EOS for dense neutron-rich matter in neutron stars was identified as an important scientific objective in the 2002 and 2007 Long Range Plans for Nuclear Science. Heavy-ion reactions induced by neutron-rich nuclei have a crucial role to play in reaching this objective. Recent and planned experiments are setting constraints on the symmetry energy at densities and temperatures away from normal nuclear matter. [Preview Abstract] |
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