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 BA: Plenary II
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Chair: Tomofumi Nagae, Kyoto University
Room: Hilton Monarchy Ballroom
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Wednesday, October 24, 2018
11:00AM - 11:45AM
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BA.00001: Exploring towards the nuclear limit: neutron drip line and beyond
Invited Speaker:
Takashi Nakamura
How many neutrons can be added to a bound nucleus before it becomes unbound? The location of the neutron drip line, the bound limit in the neutron-rich side in the nuclear chart, is indeed one of the fundamental unsolved questions in nuclear physics, as this is established experimentally only up to Z=8. The other question we address here is how atomic nuclei behave near the drip line and beyond. With these questions in mind, I present and discuss the recent experimental studies on exotic neutron-rich nuclei using RIBF (RI-Beam Factory) at RIKEN, which may be the most advanced rare-isotope beam facility in the world [1]. Neutron-rich nuclei, in particular near and beyond the neutron-drip line, show characteristic structure due to the weakly-binding (or unbinding), and large difference between neutron and proton Fermi energies. Key aspects are the nuclear shell evolution, deformation, continuum effects, neutron halo, and the strong two neutron correlations called dineutrons, which are discussed. Here, I will focus on the results on nuclei near/beyond the neutron drip line, using SAMURAI facility at RIBF. Finally, I will provide perspectives on experimental studies using the new-generation RI-beam facilities along the neutron drip line. [1] T.Nakamura, H. Sakurai, H. Watanabe, Prog. Part. Nucl. Phys. 97, 53 (2017). |
Wednesday, October 24, 2018
11:45AM - 12:30PM
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BA.00002: Heavy Elements and Fundamental Physics from Neutron Star Mergers
Invited Speaker:
Daniel Kasen
Just over one year ago, the merger of two neutron stars was detected in both gravitational and electromagnetic radiation. The unprecedented event illuminated the fundamental physics of gravity and dense matter and addressed long standing questions as to the cosmic origin of the heavy elements. I will review our understanding of mergers -- grounded in theoretical simulations and experimental data -- and will describe how material expelled in these events can assemble into heavy nuclei via rapid neutron capture (the "r-process"). The radioactive glow of these freshly synthesized isotopes allows us to directly study r-process elements at their production site. I'll explain how joint observations of gravitational waves, high energy photons, and optical/infrared emission can be used to constrain the speed of gravity, the equation of state of dense matter, and the formation of heavy nuclei, and will look ahead to what future "multi-messenger" observations, combined with data from nuclear experiments, can tell us about the physics of compact object mergers and the cosmic origin of the heavy elements.
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