Rare Isotopes ISOTOPES discovery https://www.youtube.com/watch?v=ZvuMRwvJhHw&spfreload=10
How did visible matter come into being and how does it evolve? The radioactive galaxy demonstrates the continuing formation of new radioactive isotopes A 'snapshot' view of ongoing nucleosynthesis in the Galaxy by COMPTEL and INTEGRAL … 26 Al distribution along galactic plane T =7.2 · 10 5 yr E γ =1.809 MeV The mean lifetime of 26 Al makes the 1.809 MeV gamma-ray line an excellent tracer for newly synthesized material released into the interstellar medium over the last several million years
How are atoms cooked in the Cosmos? Chemical evolution LOFT (early 2020s ?, ESA) Hubble Swift Chandra r-process Most elements are created in violent stellar explosions, and orbiting and Earth-based NuSTAR telescopes are capable of measuring these Keck creation rates. rp-process To interpret observations, however, we must understand reactions occurring in stellar explosions that create and destroy rare isotopes. Reaction networks n-star crust (captures, decays) Apache Point processes LSST (High Priority ASTRO 2010) FRIB, TRIUMF, RIBF, …
Chemical evolution mass fraction Big oldest solar system r-process 10 -3 Bang stars 10 -6 10 -9 10 -12 0 50 0 50 100 0 50 100 150 200 0 50 100 150 200 mass number supernova neutron star merger entropy http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=10543 velocity S. Bruenn et al., ApJ 767, L6 (2012) S. Rosswog et al., MNRAS 430, 2585 (2013)
Half of the neutron-rich atomic nuclei heavier than iron are built by neutron driven r-process. The final abundances reflect the shell structure of nuclei, which determines the respective nucleosynthesis trajectories. Curiosity Mars Rover – powered by 238 Pu
Quest for understanding the neutron-rich matter on Earth and in the Cosmos Data Crustal structures Bounds on EOS Symmetry energy slope EOS with hyperons Symmetry energy
The crucial role of High Performance Computing Future: large multi-institutional efforts involving strong coupling between physics, computer science, and applied math Towards predictive capability W. Nazarewicz 30
hLp://compuZngnuclei.org ¡ ¡ ¡ fusion ¡ Validated ¡Nuclear ¡ InteracZons ¡ Op4miza4on ¡ Chiral ¡EFT ¡ Model ¡valida4on ¡ Ab-‑ini4o ¡ Uncertainty ¡Quan4fica4on ¡ Neutron ¡drops ¡ Structure ¡and ¡ReacZons: ¡ Structure ¡and ¡ReacZons: ¡ ¡ Light ¡and ¡Medium ¡Nuclei ¡ Heavy ¡Nuclei ¡ EOS ¡ Correla4ons ¡ Stellar ¡burning ¡ DFT ¡ Load ¡balancing ¡ Ab-‑ini4o ¡ Load ¡balancing ¡ TDDFT ¡ Op4miza4on ¡ RGM ¡ Eigensolvers ¡ Model ¡valida4on ¡ CI ¡ Nonlinear ¡solvers ¡ Uncertainty ¡Quan4fica4on ¡ Model ¡valida4on ¡ Eigensolvers ¡ Uncertainty ¡Quan4fica4on ¡ Nonlinear ¡solvers ¡ ¡ Mul4resolu4on ¡analysis ¡ ¡ ¡ Neutrinos ¡and ¡ Fission ¡ Fundamental ¡Symmetries ¡ Neutron ¡Stars ¡
60 Progress in ab-initio calculations 50 40 A 30 20 10 0 1980 1990 2000 2010 2020 Year
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