ILE, Osaka University ILE, Osaka February 3, 2014

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1 Summary of Today s Workshop Hideaki Takabe (Aki) ILE, Osaka University ILE, Osaka February 3, 2014

2 Brief Summary Basic Science on (Astrophysics) Nuclear Physics with ps and ns Intense Lasers 1. NEEC (NEET) b-f process - Nuclear excitation (b-b: NEET) Plasma is essential 2. Neutron Source PW Laser - MeV Protons - MeV neutrons 3. NS-NS Merging Many r-process synthesis - Event rate (1/100 enough) 4. Many Mysteries Neutrino driven reactions. 6 Li problem - Photo-nuclear reaction etc.

3 Number Abundance (Si = 10 6 ) Solar System Abundance n-, g- & n- induced nuclear reactions play the significant roles in explosive element genesis! Big-Bang Nucleosynthesis 1,2 H, 3,4 He, 6,7 Li, etc. Stellar Fusion 12 C 56 Fe- 58 Ni, etc. (r-nuclei) (s-nuclei) Core-Collapse SNe & AGB: 56 Fe < A Iron peak Core Collapse Supernova n-processes r-nuclei 7 Li, 11 B np-nuclei 232 Th (14.05Gy) 238 U (4.47 Gy) B Cosmic Ray Spallation Li-Be-B, F, Na, etc. p-nuclei 92 Nb 98 Tc 138 La 180 Ta Mass Number A

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5 Nucleosynthesis of heavy elements by photons in supernova explosions The p-nuclei are synthesized by two subsequent photon-induced reactions in O/Ne layers in supernova explosions

6 Type II SN Explosion Simulation

7 Luca Baiotti et al,

8 R and S Processes

9 Evolution of stars of different masses are represented in the Hertzsprung Russell diagram. The asymptotic giant branch is marked AGB in the case of a star of 2 solar masses.

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11 r and s Processes in Astrophysics

12 Nuclear chart known: ~3,000 predicted: ~10,000 (7,000) Z (proton) + fission - ~300 Aug N (nuetron) APPC10

13 Nucleon density neutron 11 Li 208 Pb proton Stable nuclei Hallo Nucleus skin n-rich hallo drip-line excess neutrons: decoiupled strog p-n interaction by Tanihata.

14 Double decay - n mass - Astro-Cosmology Connection K. Yako et al., PRL 103 (2009) Experiment (RCNP, Osaka) Shell model (theory)

15 Nuclear-Plasma Interactions (NPI) can excite nuclear states with energies comparable to those of the surrounding plasma Photo-absorption Time Reverse: g-ray decay Well understood Atomic-nuclear (electron) interactions NEEC, NEET, IES Time Reverse: IC-decay e free/boun e free/bound d N Radiative Dielectronic N* Photons N B(E/M l) N* HEDP electrons Atom photons Nucleus Recombination Photons F(E g ), r(e x,j π ) NEET: measured once * NEEC: never observed *Phys. Rev. Lett (2000), Phys. Rev. C R (2006)

16 Counts 1 6 The 9.7 hour 12 - isomer in 196 Au might allow us to explore the interaction of highly-excited states with a HEDP 197 Au(n,2n) 196m Au 197 Au(n,2n) 196g Au This is entirely new Nuclear Physics N SRC data DT cryo with Y 14 =5x S n =6.642 MeV 100 Energy (kev) r 1 ev -1 { G 1 ev 197 Au 196 Au { r 1 ev -1 Vacant electron orbital

17 Unresolved Transition Array Fe Opacity: OPAL By Roger, Iglesias, Wilson

18 TNSA proton based nuclear-plasma experiment make 196m,g Au using the 198 Pt(p,3n) reaction Use TNSA protons from a petawatt laser to make an excited nucleus via the 198 Pt(p,3n) 196m,g Au 1 mm P t f o i l Use a long pulse (ns) laser to place the target nuclides into an HED plasma state a fixed amount of time after the TNSA protons arrive First experiment: Platinum in a plasma state when the protons hit Control experiment: Platinum put into a plasma state after the protons hit This experiment is well-suited to laser facilities such as GEKKO-XII+LFEX

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21 Nuclear Fusion in the Sun CNO-cycle pp-chain

22 Figure: The astrophysical S-factor for the reaction 3 He( 3 He,2p) 4 He. The filled circles were obtained by an underground pilot experiment (LUNA) at the Gran Sasso facility. The solid or dashed curves indicate the inclusion (non-inclusion) of screening corrections. The Gamov peak marks the energy range probed under solar burning conditions, reached for the very first time by experiment

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25 Vacuum Breakdown and Pair-Plasma Creations with Ultra-Intense Lasers Hideaki Takabe and Toseo Moritaka Institute of Laser Engineering Yamada-oka 2-6, Suita Osaka , Japan Osaka University, International Conference on Plasma Science and Applications, 4-6 December, 2013, Singapore

26 Science on NIF Committee just after the Evaluation July 15, 2010 at LLNL David Arnett*, University of Arizona Riccardo Betti, University of Rochester Roger Blandford, Stanford University Nathanial Fisch, Princeton University Ramon Leeper, Sandia National Lab. Christopher McKee, UC Berkeley Mordecai Rosen, LNL Robert Rosner, The Univ. of Chicago (Chair) John Sarrao, Los Alamos National Laboratory Hideaki Takabe, ILE, Osaka University Justin Wark, University of Oxford Choong-Shik Yoo, Washington State University 26

27 My Conclusion Plasma Nuclear Physics is New Discipline to Make Astrophysical Nucleosynthesis Precision Science The First Challenge with Laser looks NEEC, where Plasma is Essential Process. PW Laser Protons are Source of Monoenergetic Neutron Source Where will Such research Done in a Few Years?

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