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Nuclear Physics and Astrophysics of Neutron-Star Mergers and Supernovae, and the Origin of R-Process Elements
Understanding r-process requires a significant amount of nuclear physics input both experimentally and theoretically and of astronomy input, too. Already many rare ion beam facilities, either currently operating or under construction, and astronomical observatories devote significant amount of resources. This workshop aims to bring nuclear theorists, experimentalists and astronomers together for critically discussing open questions on the r-process. Among these are 1) calculating the binding energies and reaction rates in the r-process path, 2) the spin-isospin response in a broad range of nuclei from stable isotopes to rare ions, 3) the many-body techniques required to solve the neutrino transport and flavor evolution, and 4) spectroscopic and bolometric data on neutron-capture elements in various supernova environments (i.e. near the proto-neutron star or in the outer shells) or merging neutron star binaries.
|T. Kajino||National Astronomical Observatory of Japan & University of Tokyo|
|Wako Aoki||National Astronomical Observatory of Japan|
|A. Baha Balantekin||University of Wisconsin-Madison (USA)|
|M. Tanaka||National Astronomical Observatory of Japan|