1. Neutrino-Nucleus Reactions and Nucleosynthesis Toshio Suzuki Nihon University Roles of ν-process in nucleosynthesis 核物理から見た宇宙 New Era of Nuclear Physics in The Cosmos RIKEN Sept. 25, 2008

2. Roles of ν-processes in nucleosynthesis Production of elements: 7 Li, 11 B, 19 F, 26 Al … 51 V Rare elements 138 La, 180 Ta Woosley et al, Astrophy.J 356 (1990) Heger et al., PL B606 (2005) HaxtonHeger et al.

3. Nucleosynthesis through neutrino-induced reactions Qian, Haxton, Langanke, Vogel ， PR C55 (1997) GT exp. RCNP ( 3 He, t) More GT strength than RPA (Heger et al.) Byelikov et al., PRL 98 (2007) ・ Production of rare elements by ν- reactions ・ Role of νin r-process nucleosynthesis N=82, 126 regions Withν-induced n emission →solar abundances Calculation by Heger et al.

4. Research subjects (1) Reaction rates: better evaluations ν-nucleus reaction cross sections BR to n, p, γ, αemission channnels (2) ν-oscillation effects (3) Find possible new processes ex. νp process Frohlich et al, PRL 96 (2006) 64Ge(n,p) → nucleosynthesis of A>64 nuclei 92,94Mo, 96,98Ru otherwise flow stops at 64Ge (beta halif life=64s)

5. New evaluation of reaction rates in p-shell and fp-shell nuclei ν- 12 C, ν- 4 He reactions evaluated by new shell model Hamiltonians (SFO) ・ Synthesis of 7 Li, 11 B in supernovae ・ Oscillation effects GT strength in 56 Ni, 58 Ni and Ni isotopes evaluated by GXPF1 ・ ν- 56 Ni reaction and synthesis of 55 Mn in Pop. III star ・ n emission from n-rich Ni isotopes

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

7. Supernovae νSpectra σ ∝ E 2 & tail part

8. Neutrino-induced Reactions charged-current neutral-current Spin-dependent excitations ● Gamow-Teller (1+): ● Spin-diole (0-, 1-, 2-):

9. SFO: good description of magnetic moments, GT in p-shell nucelei Suzuki, Fujimoto, Otsuka, PRC (2003) Cross sections for Supernova Neutrinos with temperature T p and n emissions BR: Hauser-Feshbach model

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

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

12. Abundances of 7 Li and 11 B produced in supernova explosion processes M=16.2 M ☼ (SN 1987A) No oscillation case Cf. Yoshida, Suzuki, Chiba et al., Astrophys. J (2008)

13. 7 Be, 11 C abundance SN Nucleosynthesis with Neutrino Oscillations Supernova nucleosynthesis ( -process) 16.2 M star supernova model corresponding to SN 1987A Increase by a factor of 2.5 and 1.4 Increase in the rates of charged-current reactions 4 He ( e,e - p) 3 He and 12 C ( e,e - p) 11 C in the He layer Normal mass hierarchy, sin 2 2  13 = 0.01 no mix mix no mix mix

14. 7 Li/ 11 B Dependence on Mass Hierarchy and  13 N( 7 Li ) / N( 11 B ) Good indicator for neutrino oscillation parameters normal inverted no mix (T e, T e, T , E ) = (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, ×10 53 ergs) Including uncertainties in neutrino temperatures N( 7 Li )/N( 11 B ) > 0.8 Normal mass hierarchy and sin 2 2  13 > 0.002 Possibility for constraining mass hierarchy and lower limit of the mixing angle  13. Neutrino experiments Constraining upper limit of  13 Cf. Yoshida et al., PRL 96 (2006)

15. 8-12MeV 8-13MeV M1 strength (GXPF1J) 7-12MeV Honma fp-shell B(GT) for 58Ni Exp: Fujita et al.

18. Neutron emission from Ni isotopes (BR by Higashiyama)

19. Neutral current reaction on 56 Ni

20. Synthesis of Mn in Population III Star

21. [Mn/Fe] No ν -0.53 HW02 -0.29 [Mn/Fe] GXPF1J -0.25 GXPF1J×2 -0.17 No ν With ν(GXPF1J) With ν x2 With ν(Woosley) Yoshida, Umeda, Nomoto

22. Summary Successful description of spin modes in nuclei （ GT transitions, magnetic moments 、 and M1 transitions ） by new shell model Hamiltonians Enhancement of ν-nucleus reaction cross sections More n emission from n-rch Ni isotopes Enhancement of production yields of 7 Li, 11 B, and 55 Mn in supernovae

23. Collaborators T. Yoshida b, S. Chiba c, M. Honma d, K. Higashiyama e, H. Umeda f, K. Nomoto f, D.H. Hartmann g, T. Kajino b,f and T. Otsuka h b National Astronomical Observatory of Japan c Japan Atomic Energy Agency d University of Aizu e Chiba Institute of Technology F Department of Astronomy, University of Tokyo g Dept. Of Physics and Astronomy, Clemson University h Department of Physics and CNS, University of Tokyo

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

25. Exp: LSND PR C64 (2001) EXP Allen et al. (1990) ν- 12 C Exclusive 12 C → 12 N (1 + ) ● WBP: Warburton-Brown ● HT: Hayes-Towner, PR C62, 015501 (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) ● SFO*: g A eff /g A =0.95 Suzuki, Chiba, Yoshida, Kajino, Otsuka, PR C74 (2006)