1. Nucleosynthesis by the Radioactive Isotope Beam and Origin of Matter (Nuclear Abundance)
Myung-Ki Cheoun
Department of Physics,
Soongsil University, Seoul, Korea
K.S.Kim, E. Ha, W.Y.So, S.Y. Lee, C. Ryu…
T.Kajino, T.Yoshida, T.Yasudake, K. Nakamura
T. Nishimura, T.Maruyama.. (NAO of Japan)
F.Simkovic, A.Faessler.. (Tuebingen)

2. Contents 0. Motivation in Nuclear Abundance
Brief Introduction of Nuclear Structure (by QRPA and Deformed QRPA)
2. Neutrino process for the origin of a proton-nucleus for 138Ce,136Ce and 180W
3. Results and Summary
Changwon, KPS 2009

3. Motivation 1
Understanding of origin of matter in the universe is strongly related with the evolution of stars, in which most of nuclei are believed to be synthesized and emitted by various explosion mechanisms at their last stages. 
The nucleosynthesis is sensitive on the given conditions of the site, such as preceding matter, temperature, masses of stars and so on, as well as Galaxy Chemical Evolution and Cosmic Ray.
Changwon, KPS 2009

4. Motivation 2
Since nuclear reactions relevant to the processes are presumed as thermally balanced, the nuclei unstable at the present time and their structure can play important roles in the nucleosynthesis.
Radioactive isotope beam facility could produce the exotic unstable nuclei and investigate their key reactions on the ground, so that it could give invaluable microscopic understanding of the origin of matter complementary to the observational astronomical data.         
Changwon, KPS 2009

5. Motivation 3
In this talk we present a few examples of origin of matter with results available from astronomical observational, experimental and theoretical data.        
Changwon, KPS 2009

6. Nucleosynthesis of Solar System (Solar Abundance) and other stars
Chondrites are stony meteorites that have not been modified
due to melting or differentiation of the parent body
Changwon, KPS 2009

7. Solar system Supernovae Model BIG-BANG STARS COSMIC-RAYS SUPERNOVAE ?
R-PROCESS
　　　　　 AGB STARS
　　　　　　　　　　　　　　　　　S-PROCESS R
S（N=50) R
S（N=82)
S（N=126) R
Actinide
COSMIC-RAYS ++ +
232Th (14.05Gy) P
238U (4.47 Gy)
Changwon, KPS 2009
SPERNOVA-g PROCESS ?

8. Universality and Anomaly !!
Changwon, KPS 2009

9. Mechanism of Super Nova Explosion
Within a massive, evolved star (a) the onion-layered shells of elements undergo fusion, forming an iron core (b) that reaches Chandrasekhar-mass and starts to collapse.
The inner part of the core is compressed into neutrons (c), causing infalling material to bounce (d) and form an outward-propagating shock front (red). The shock starts to stall (e), but it is reinvigorated by neutrino interaction.
The surrounding material is blasted away (f), leaving only a degenerate remnant.
Changwon, KPS 2009

10. SUPERNOVA R-PROCESS t = 0 Neutrino-driven wind formsPb ○
SUPERNOVA R-PROCESS
Otsuki, Tagoshi, Kajino & Wanajo
2000, ApJ 533, 424
Wanajo, Kajino, Mathews & Otsuki
2001, ApJ 554, 578 Z Fe ○ N
　t = 0
　Neutrino-driven wind forms
　right after SN core collapse.
　 n + p n + a
　t = 18 ms
Seeds form.
Exotic neutron-rich 78Ni
　t = 568 ms – 1 s
Heavy r-elements synthesize.　
Pb208 ○
Fe56 ○
Ni78 Pb ○ Fe ○
Changwon, KPS 2009

11. Origin of Proton-nuclei
138La and 180Ta show an anomaly !!
Changwon, KPS 2009

12. Origin of P-nucleus Hayakawa, PRL, 2004
Neutrino-process could be important !!
Hayakawa, PRL, 2004
Changwon, KPS 2009

13. Nuclear Structures and relevant reactions (neutrino process)
139La(ν,ν'n)138La
N=82, Magic Number
Changwon, KPS 2009

14.
Changwon, KPS 2009

15. How to understand exotic nuclear structure and
How to pin down the ambiguities from the structure?
Changwon, KPS 2009

16. Typical cross section by incident neutrino and electron
Giant Resonance
Delta Resonance
Quasi Elastic Region
Hadronic Region
energy
N* Resonance
Dip Region
Discrete
Excited states
Pion Threshold q
Typical cross section by incident neutrino and electron
Changwon, KPS 2009

17. How to describe the ground and excited states ?
ν’(l)
Indirect (Two-step) Processes ν
W(+,-), Z0
p,n,… A* A B
How to describe the ground and excited states ?
J ∏ A* A
Changwon, KPS 2009 B

18. Results : Neutrino Inclusive Reactions for 138Ba via CC and139La via NC
Changwon, KPS 2009

19. Key Reactions for 138La : Neutral Current
139La(ν,ν'n)138La
These excited states are of importance
for this reaction.
This state is populated in SNe of T9=1-3.
The population ratio is calculated by T. E.
N=82, Magic Number
Changwon, KPS 2009
By Dr. Hayakawa

20.
Changwon, KPS 2009

21. Can reproduce experimental (GT) by quenching !!
(5.56,3.15)
(3.88,4.5)
Changwon, KPS 2009

22. Dominated by 1+ ?? !!
Changwon, KPS 2009

23. Our QRPA can reproduce exp. Data !!
Changwon, KPS 2009

24.
Changwon, KPS 2009

25. Summary and Remarks
Astronomical Observational data with meteorite analysis show nuclear abundances in solar and other stars, which show a universality. Origins for part of them are not clear still.
As an example, origin of 138La and Ta180 leading to the proton-nucleus 180W and 136Ce are studied by their relevant nuclear reactions, in specific, neutrino reactions are detailed by experiments and theoretical calculations. Network calculations are in progress.
Changwon, KPS 2009

26. Origins of matter (nuclear abundances) Exotic Nuclear Structure
RI beam experimental
data
Exotic Nuclear Structure
Calculations
Astronomical
Observational data
Changwon, KPS 2009

27. Special thanks to the O.C. for pioneering symposium
In this KPS !!
감사합니다 !!
Changwon, KPS 2009