Nuclear Physics Sakura-i Hiro-yoshi 櫻井博儀 Fundamental

Nuclear Physics Sakura-i　　Hiro-yoshi 櫻　　　井　博儀

Fundamental interactions Elementary particles Composite particles

Q. 1 Life time of neutron？ Q. 2　Age of universe is 13. 7 B Years after Big. Bang. there are neutrons in materials. Why? Q. 3 Spin-parity for ground state of deuteron？ Q. 4　Limits of existence of nuclei？ Q. 5 Magic numbers of nuclei？ Q. 6　Size of nuclei？ Q. 7　Collective motions of nuclei？ Q. 8　How and where elements around us have been created ? 　

Exploration of the Limit of Existence stable nuclei unstable nuclei observed so far drip-lines (limit of existence)（theoretical predictions) magic numbers in 1995 ~300 nuclei ~2700 nuclei ~6000 nuclei proton drip-line proton-rich nuclei proton number (Z) neutron drip-line neutron-rich nuclei in 1985 neutron number (N)

Nuclear Collective Motion closed shell at magic number spherical nuclei |b|~0 open shell surface vibration Quadrupole deformation parameter b deformed nuclei |b| large degree of collectivity E(4+)/E(2+) ~ 1. 8 ~ 2. 2 ~ 3. 3

Solar Abundance of Elements Big Bang Nucleosynthesis in stellars (fusion） Nucleosynthesis in r-process path 金 T. Motobayashi

Gold・・・

r-process path in supernova explosion Photo-disintegration of ion nuclei Electron capture reaction Proton number 陽子数 Emission of big amount of neutron and neutrino Au Beta decay Z, N -> Z+1, N-1 r-process Neutron capture Beta decay Neutron number 中性子数 Fe to U

Exploration of the Limit of Existence stable nuclei unstable nuclei observed so far drip-lines (limit of existence)（theoretical predictions) magic numbers in 1995 ~300 nuclei ~2700 nuclei ~6000 nuclei proton drip-line proton-rich nuclei proton number (Z) neutron drip-line neutron-rich nuclei in 1985 neutron number (N)

New frameworks for the new region of nuclear chart Nuclear Structure: Shell evolution Nuclear Matter: New forms Stable Nuclei Neutron-rich Nuclei ? neutron-skin nuclei ? ? neutron-halo nuclei N=16 N=6 11 Be, 11 Li, 19 C. . . To write up new text book： Exotic phenomena, Systematics, etc. Isospin-, density-dependences of effective interactions, nucleon-corrections Microscopic system (nuclei) to Macroscopic system (neutron stars)

Challenge for r-process path and explosion in supernovae Synthesis up to U （r-process）　　unknown neutron-rich nuclei 　 theoretical predictions only Necessary of experimental investigation for nuclear properties of heavy and neutron-rich nuclei Mass, life-time, decay mode Mass number Explosion mechanism of supernova 　　No explosion in theoretical works 　　Outer clast of neutron star Necessary of experimental study for Equation-of-State for nuclear matter 1987 A 5

Challenge to investigate EOS of neutron matter E/A [Me. V] from nuclei to neutron stars Normal density r 1 S (fm-3) correlation BCS-BEC crossover in dilute system (r ~ 0. 1 r 0) ? 3 NF 　 T=3/2 channels? 　 density dependence? 3 P correlation 　　pairing gap? Density depencence? 2

Nuclear Physics is not Particle Physics, not Condensed Matter Physics Interaction? Effective interaction ? Correlations ? Isospin, Density, temperature dependences ? Surface boundary, non-linear, finite system

RIKEN RI Beam Factory (RIBF) Experiment facility Old facility To be funded Accelerator RIPS ~100 Me. V/nucleon GARIS SHE (eg. Z=113) ~5 Me. V/nucleon RILAC SCRIT AVF f. RC Zero. Degree RRC SAMURAI SRC SLOWRI RI-ring IRC CRIB (CNS) New facility Big. RIPS SHARAQ 350 -400 Me. V/nucleon Intense (80 k. W max. ) H. I. beams (up to U) of 345 AMe. V at SRC Fast RI beams by projectile fragmentation and U-fission at Big. RIPS Operation since 2007

Exploration of the Limit of Existence Great expansion of nuclear world by RIBF Intensity > 1 particle/day (EPAX@GSI) protons New Element 278 113 04 July 23 18: 55 57 fb Projectile Fragmentation In-flight U fission & P. F. 78 Ni ~0. 1 particles/sec. (goal) 10 particles/sec. (2007) by 10 pn. A 350 Me. V/u U-beam by 1 pm. A neutrons

RI beam production via in-flight method RI production RI beam separator （to collect and separate RI with analyzing magnets） Heavy ion accelerator target （to accelerate nuclei）（to make reactions 　Be, C, etc） Advantage of fission via U beam RI beam Probability Fission reaction via 238 U beam N=50 Yield rate of 78 Ni via fission is about 1､ 000 times higher than via fragmentation. 10, 000: 1 Fragmentation reaction via 86 Kr beam 78 Ni Proton number

RI Beam Facilities in the world Finland JYFL Germany GSI Russia JINR China IMP CIAE France GANIL SPIRAL-I, II (2010 -) SISSI+LISE Canada TRIUMF/ISAC USA MSU/NSCL ORNL/HRIBF ANL Texas A&M Switzerland CERN/ISOLDE Italy LNS Japan RIKEN KEK-JAEA/TRIAC India VECC IUAC Red colored: In-flight method

RIB Facilities in the Middle East and East Israel Soreq NRC SARAF India VECC RIB project China IMP HIRFL CIAE BRNBF Japan RIKEN RIBF CNS, U. -Tokyo CRIB KEK-JAEA TRIAC, RMS RCNP, Osaka-U EN-course CYRIC, Tohoku-U RF-IGISOL HIMAC

Applications of Nuclear Physics

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Nuclear Physics Sakura-i Hiro-yoshi 櫻 井 博 儀 Fundamental

Nuclear Physics Sakura-i Hiro-yoshi 櫻井博儀 Fundamental