1. Neutrino-Nucleus Reactions and Nucleosynthesis
Toshio Suzuki Nihon University/CNS
・Neutrino-induced reactions on 12C and 4He
　　 based on new shell-model Hamiltonians
　　・Synthesis of light elements during supernova
explosion Li, 11B etc.
2. ・Neutrino-induced reactions on Fe and Ni isotopes
based on new shell-model Hamiltonian (GXPF1)
・Synthesis of heavier elements e.g. 55Mn

2. Collaborators T. Otsuka, University of Tokyo/CNS, RIKEN S. Chiba, JAEA
M. Honma, University of Aizu
K. Higashiyama, Chiba Institute of Technology
T. Yoshida, NAO
H. Umeda, University of Tokyo
K. Nomoto, University of Tokyo
T. Kajino, NAO/University of Tokyo
R. Fujimoto, Hitachi Co.

3. Neutrino induced reactions
on 12C and 4He
○ New Shell-Model Hamiltonian
in p-sd shell: SFO
Suzuki, Fujimoto & Otsuka, PR C67, (2003)
・Enhanced spin-isospin interactions
Proper tensor components
・ Improved spin and magnetic properties
Proper shell evolution

4. B(GT) values for 12C -> 12N
Magnetic moments of p-shell nuclei
SFO
B(GT) values for 14N -> 14C
SFO
present = SFO Suzuki, Fujimoto,
Otsuka, PR C67 (2003)
Negret et al., PRL 97 (2006)
KVI
RCNP
SFO*: gAeff/gA=0.95
B(GT: 12C) fitted to experiment

5. Effects of Tensor Force on Shell Evolution
Otsuka, Suzuki, Fujimoto, Grawe, Akaishi, PRL 69 (2005)
Effective Single-Particle Energy
　　　　　 for N=8 Nuclei

6. ○ Neutrino induced reactions on 12C
・Exclusive and inclusive reactions by DAR
・Reactions induced by supernova
○ Reactions on 4He
○ Synthesis of light elements; 7Li, 11B etc.
・Dependence of production rates on shell
model Hamiltonians
・Constraints on neutrino temperatures
・Effects of neutrino oscillations

7. DAR ν spectra Exclusive 12C → 12N (1+) EXP ●SFO*: gAeff/gA=0.95
Allen et al.
(1990)
Exp: LSND
PR C64 (2001)
●SFO*: gAeff/gA=0.95
　Suzuki, Chiba, Yoshida, Kajino, Otsuka,
　　PR C74 (2006)
●WBP: Warburton-Brown
●HT: Hayes-Towner, PR C62, (2000)
p:Cohen-Kurath (8-16)2BME, sd: USD of Wildenthal, 　
pf: KB3, p-sd and others: Millener-Kurath
●NCSM: Hayes-Navratil-Vary, PRL 91 (2003)　
AV8’(2-body) + TM’(99) (3-body)
●CRPA: Kolb-Langanke-Vogel, NP A652, 91 (1999)

8. Inclusive = Exclusive (1+g.s.) + Excited state
Exp:
LSND
PR C64 (2001) 2-
2－: gAeff/gA = * 0.75 *0.70
Cf. Gaarde et al.
q= (CK)
Quenching of spin-dipole strength

9. Cross sections for Supernova Neutrinos with temperature T
Proton and neutron
emissions　BR:
Hauser-Feshbach model

10. Cross sections for Supernova Neutrinos with temperature T S. Chiba

11. Light Element Abundances and Nucleosynthesis Processes
Inner O/C He/C He/H H

12. ν- 4He reaction cross sections
cf. Woosley-Haxton: Sussex potential by Elliott et al.

13. Effects of the spreading of the SD strength
Nakayama et al.
SPSDMK*
GDR+SDR1+SDR2

14. Abundances of 7Li and 11B produced in supernova explosion processes
　　M=16.2 M☼ (SN 1987A)
No oscillation case

15. Constraints on neutrino temperatures
SN contributions in GCE:
WBP+SFO
WBP+SFO
SPSDMK+PSDMK2
Yoshida, Kajino, Hartmann,
PRL 94 (2005)

16. SN Nucleosynthesis with Neutrino Oscillations
Supernova nucleosynthesis (n-process)
16.2 M star supernova model corresponding to SN 1987A
Normal mass hierarchy, sin22q13 = 0.01
no mix
mix
7Be, 11C abundance
Increase by a factor of 2.5 and 1.4
Increase in the rates of charged-current reactions
4He(ne,e-p)3He and 12C(ne,e-p)11C in the He layer

17. 7Li/11B Dependence on Mass Hierarchy and q13
N(7Li)/N(11B)
Good indicator for neutrino oscillation parameters
normal
inverted
no mix
Including uncertainties in neutrino temperatures
(Tne, Tne, Tnm,t, En)
= (3.2, 5.0, 6.0, 3.0)
, (3.2, 4.8, 5.8, 3.0)
, (3.2, 5.0, 6.4, 2.4)
, (3.2, 4.1, 5.0, 3.5)
, (4.0, 4.0, 6.0, 3.0)
, (4.0, 5.0, 6.0, 3.0)
(MeV, MeV, MeV, ×1053ergs)
Normal mass hierarchy and sin22q13 > 0.002
Cf. Yoshida et al.,
PRL 96 (2006)
N(7Li)/N(11B) > 0.8
Possibility for constraining mass hierarchy and
lower limit of the mixing angle q13.
Neutrino experiments
Constraining upper limit of q13

18. 2. Neutrino Nucleus Reactions on Fe and Ni Isotopes
Charge-exchange and neutral-current reactions;
● Gamow-Teller transitions
GT strength: shell model calculation by Honma
et al GXPF1J
● Emissions of proton, neutron, α, γ
● Production of Mn in Population III star

19. M1 strength (GXPF1J) B(GT) for 58Ni Honma Exp: Fujita et al. 8-13MeV

20. B(GT)=9.47 B(GT)exp=9.9±2.4 B(GT)KB3G=8.86 GXPF1J Honma et al.
cf. KB3 Caurier et al.
B(GT)= B(GT)exp=9.9±2.4
B(GT)KB3G=8.86

21. Neutral Current Reactions GT0

22. Neutral Current Reactions

23. Synthesis of Mn in Population III Star

24. Yoshida, Umeda, Nomoto
　　　　[Mn/Fe]
No ν HW
　　　 [Mn/Fe]
GXPF1J
GXPF1J×
KB3G
KB3G×2　
No ν
With ν(GXPF1J)
With ν x2
With ν(Woosley)

25. Summary
New shell-model Hamiltonian (SFO) with a proper role of spin-isospin interaction and shell evolustion
Better description of Gamow-Teller transitions and magnetic moments in p-shell
Applications to neutrino-nucleus reactions on 12C and 4He
Enhanced cross sections -> enhanced yields of light elements during supernova explosion: 7Li, 11B, 10Be etc.
Constraints on neutrino temperatures
Constraint on ν mass hierarchy and lower limit on
Larger strength with more fragmentation for GXPF1 than KB3G in GT strengths in Fe and Ni isotopes
Enhancement of neutral current reaction cross sections in Fe and Ni isotopes -> Enhancement of synthesis of Mn and Co by neutrino processes