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 4WFA: Science of Intense High Energy Rare Isotope Beams IInvited Workshop
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Chair: Tadaaki Isobe, RIKEN Nishina Center Room: Hilton Waikoloa Village Queens 5 |
Monday, November 27, 2023 2:00PM - 2:30PM |
4WFA.00001: Probing the EOS of neutron stars with heavy ion collisions Invited Speaker: Kyle W Brown The nuclear equation of state (EoS) underpins our knowledge of how nucleons assemble themselves from finite nuclei to neutron stars. The nuclear and astrophysical communities are taking a multifaceted approach to studying this important relation: from ground and space-based observations of neutron stars and their mergers to laboratory measurements of nuclear reactions and electron scattering. The past few years in particular have seen a number of high-profile measurements on the equation of state from these approaches. With the next generation accelerator facilities coming online, the nuclear science community is poised to further improve our understanding of the nature of neutron-rich nuclear matter with terrestrial measurements. The Facility for Rare Isotope Beams (FRIB) will provide a unique opportunity to study the nuclear equation of state at both super-saturation density, as well as large isospin asymmetry. This is particularly true as we look forward to the upgrade to 400 MeV/u. |
Monday, November 27, 2023 2:30PM - 3:00PM |
4WFA.00002: New initiatives of in-beam spectroscopy at RIBF Invited Speaker: Daisuke Suzuki The RI Beam Factory (RIBF) is a third-generation in-flight facility, designed and optimized for the RI beam production by uranium fission. High intensity beams available over a wide region of the nuclear chart creates great opportunities for in-beam reaction studies at the energies around 200 to 300 MeV/u. Furthermore, three spectrometers, namely ZeroDegree, Samurai and SHARAQ/OEDO each having specific advantages, give rise to a wider spectrum of reaction studies at the RIBF. The area of reaction studies has been advanced further by new initiatives since the last meeting at Hawaii. One is that the energy-degrading RI beamline OEDO has been set for full operation. OEDO decelerates RI beams in-flight down to about 10 MeV/u, thus providing the energy tunability to bolster the versatility of reactions, which is limited at original beam energies of the RIBF. Another initiative is the HiCARI campaign at ZeroDegree, which introduced tracking-type germanium detectors, for the first time, for in-beam gamma-ray spectroscopy at the RIBF. These initiatives not only provide fruitful scientific outcomes with the current RIBF, but also lay a foundation for in-beam reaction studies toward the upgraded RIBF, where the uranium beam intensity presently limited to 100 pnA will increase to 2,000 pnA. |
Monday, November 27, 2023 3:00PM - 3:30PM |
4WFA.00003: Fission and r-process nucleosynthesis Invited Speaker: Nicole Vassh Following the dawn of multi-messenger observations enabled by LIGO we have now seen heavy element formation in the act via the signature of lanthanide elements on the observed light curve from the merger of two neutron stars. This new wave of observational capabilities provides the opportunity to make big leaps in our understanding of heavy element production over the next decade. An outstanding issue which directly impacts our interpretation of such nucleosynthesis observables lies in modeling the production of actinides in astrophysics. For instance, it remains unknown how high of a mass number astrophysical environments are able to reach before the nucleosynthesis is terminated by fission. Stellar spectroscopy and meteorites have revealed the presence of uranium, thorium, plutonium, and curium, showing that astrophysical phenomena are capable of synthesizing up to at least atomic number 96 and mass number 247. But is the rapid neutron capture process (r-process) solely responsible for the actinide content of our galaxy? And which types of astrophysical events can reach such heavy species? Recent work over the last few years has introduced several potential observables of actinide production which could shed light on these questions, from late-time fission heating effects on merger light curves, to MeV gamma-rays unique to the fission process, as well as hints of fission products in metal-poor star abundance patterns. Using observables to unravel the mystery of actinide production in astrophysics however requires careful consideration of the impact of the nuclear physics uncertainties associated with the vastly uncharted territory of neutron-rich nuclei. I will discuss potential observables of actinide production and highlight how rare isotope beam facilities like ARIEL and FRIB can contribute towards an understanding of the ultimate termination point of heavy element synthesis. |
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