Bulletin of the American Physical Society
5th Joint Meeting of the APS Division of Nuclear Physics and the Physical Society of Japan
Volume 63, Number 12
Tuesday–Saturday, October 23–27, 2018; Waikoloa, Hawaii
Session 2WAB: Nuclear Equation of State in Context of Neutron Star Merger Event II
4:00 PM–5:30 PM,
Tuesday, October 23, 2018
Hilton Room: Kona 4
Chair: Akira Ohnishi, Yukawa Institute for Theoretical Physics, Kyoto Univesity
Abstract ID: BAPS.2018.HAW.2WAB.2
Abstract: 2WAB.00002 : High-density symmetry energy and pion production in heavy-ion collisions
4:30 PM–5:00 PM
The density dependence of the nuclear symmetry energy is a valuable information for understanding neutron rich systems such as the nuclear structure, heavy-ion collisions, neutron stars and their mergers. Especially, heavy-ion collisions are believed to be useful to investigate the symmetry energy at high densities. Since the neutron-proton ratio in the high-density region is not a direct observable, the pion ratio has been proposed to be a good probe to constrain the high-density behavior of the symmetry energy.
At present, some theoretical studies have been performed by different transport models to investigate the sensitivity of pion observables in heavy-ion collisions. However, some of these results are contradicting to each other even qualitatively. Therefore, it is necessary to understand the relation between the pion ratio and the nucleon dynamics to deduce the information on the symmetry energy. In the experimental studies, Sn+Sn collisions have been performed at RIBF/RIKEN.
In this presentation, we report the results for the pion production in central collisions of neutron-rich nuclei using our transport model that combines antisymmetrized molecular dynamics (AMD) and a hadronic cascade model (JAM). In our calculation, we found the mechanism how the delta resonance and pions are produced reflecting the dynamics of neutrons and protons.
To cite this abstract, use the following reference: http://meetings.aps.org/link/BAPS.2018.HAW.2WAB.2
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