NeutrinoNucleus Reactions and Nucleosynthesis Toshio Suzuki Nihon University

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

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 B 606 (2005) Haxton Heger et al.

Nucleosynthesis through neutrino-induced reactions ・Production of rare elements by ν- reactions Calculation by Heger et al. GT exp. RCNP (3 He, t) More GT strength than RPA (Heger et al. ) Byelikov et al. , PRL 98 (2007) ・Role of νin r-process nucleosynthesis N=82, 126 regions Withν-induced n emission →solar abundances Qian, Haxton, Langanke, Vogel，PR C 55 (1997)

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) 64 Ge(n, p) → nucleosynthesis of A>64 nuclei 92, 94 Mo, 96, 98 Ru otherwise flow stops at 64 Ge (beta halif life=64 s)

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 GXPF 1 ・ν-56 Ni reaction and synthesis of 55 Mn in Pop. III star ・n emission from n-rich Ni isotopes

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

Supernovae νSpectra σ∝ E 2 <E> & tail part

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

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

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

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

Abundances of 7 Li and 11 B produced in supernova explosion processes M=16. 2 M☼ (SN 1987 A) No oscillation case Cf. Yoshida, Suzuki, Chiba et al. , Astrophys. J (2008)

SN Nucleosynthesis with Neutrino Oscillations Supernova nucleosynthesis (n-process) 16. 2 M star supernova model 2 corresponding to SN 1987 A Normal mass hierarchy, sin 2 q 13 = 0. 01 mix ix m no no mix mi x no mix Increase by a factor of 2. 5 and 1. 4 abundance Increase in the rates of charged-current reactions 4 He(n , e-p)3 He and 12 C(n , e-p)11 C in the He layer e e 7 Be, 11 C

7 Li/11 B Dependence on Mass Hierarchy and q 13 N(7 Li)/N(11 B) Good indicator for neutrino oscillation parameters Including uncertainties in neutrino temperatures normal inverted no mix (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, 6. 0, 3. 0) , (4. 0, 5. 0, 6. 0, 3. 0) (Me. V, × 1053 ergs) Normal mass hierarchy and sin 22 q 13 > 0. 002 Cf. Yoshida et al. , N(7 Li)/N(11 B) > 0. 8 PRL 96 (2006) Possibility for constraining mass hierarchy and lower limit of the mixing angle q 13. Neutrino experiments Constraining upper limit of q 13

fp-shell B(GT) for 58 Ni Exp: Fujita et al. M 1 strength (GXPF 1 J) Honma 8 -13 Me. V 7 -12 Me. V 8 -12 Me. V 7 -12 Me. V

Neutron emission from Ni isotopes (BR by Higashiyama)

Neutral current reaction on 56 Ni

Synthesis of Mn in Population III Star

Yoshida, Umeda, Nomoto [Mn/Fe] No ν -0. 53 HW 02 -0. 29 [Mn/Fe] GXPF 1 J -0. 25 GXPF 1 J× 2 -0. 17 No ν With ν(GXPF 1 J) With ν x 2 With ν(Woosley)

Summary • Successful description of spin modes in nuclei （GT transitions, magnetic moments、and M 1 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

Collaborators T. Yoshidab, S. Chibac, M. Honmad, K. Higashiyamae, H. Umedaf, K. Nomotof, D. H. Hartmanng, T. Kajinob, f and T. Otsukah b. National Astronomical Observatory of Japan c. Japan Atomic Energy Agency d. University of Aizu e. Chiba Institute of Technology FDepartment of Astronomy, University of Tokyo g. Dept. Of Physics and Astronomy, Clemson University h. Department of Physics and CNS, University of Tokyo

B(GT) values for 12 C -> 12 N B(GT) values SFO for 14 N Magnetic moments of p-shell nuclei -> 14 C SFO present = SFO Suzuki, Fujimoto, Otsuka, PR C 67 (2003) Negret et al. , PRL 97 (2006) KVI RCNP SFO*: g. Aeff/g. A=0. 95 B(GT: 12 C)_cal = experiment

ν-12 C Exclusive 12 C → 12 N (1+) Allen et al. (1990) EXP Exp: LSND PR C 64 (2001) ●SFO*: g. Aeff/g. A=0. 95 Suzuki, Chiba, Yoshida, Kajino, Otsuka, PR C 74 (2006) ●WBP: Warburton-Brown ●HT: Hayes-Towner, PR C 62, 015501 (2000) p: Cohen-Kurath (8 -16)2 BME, sd: USD of Wildenthal, pf: KB 3, p-sd and others: Millener-Kurath ●NCSM: Hayes-Navratil-Vary, PRL 91 (2003) AV 8’(2 -body) + TM’(99) (3 -body) ●CRPA: Kolb-Langanke-Vogel, NP A 652, 91 (1999)