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NUINT11, Dehradun March 9, 2011

Neutrino-Nucleus Reactions at MeV Region based on New Shell-Model Hamiltonians Toshio Suzuki Nihon University. NUINT11, Dehradun March 9, 2011. Neutrino energy: < 100 MeV Shell model: Our work is based on Recent advances in shell model calculations, owing to

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NUINT11, Dehradun March 9, 2011

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  1. Neutrino-Nucleus Reactions at MeV Region based on New Shell-Model HamiltoniansToshio SuzukiNihon University NUINT11, Dehradun March 9, 2011

  2. Neutrino energy: < 100 MeV Shell model: Our work is based on Recent advances in shell model calculations, owing to New RIBF for studies of unstable nuclei Many unstable nuclei toward and at the drip-lines are found -> Change of magic numbers toward drip-lines Magic numbers: Z, N = 2, 8, 20, 28, 50, 82, 126 (Meyer-Jensen) Vanishing of neutron magic number at 8, 20, 28 … New magic numbers: 8 -> 6 20 -> 16 etc.

  3. New evaluation of reaction rates in p-shell and fp-shell nuclei ● New shell model Hamiltonians, which give good acount of spin modes in nuclei ● ・ν-12C, ν-4He reactions evaluated by new shell model Hamiltonians (SFO, WB) 　 ・Synthesis of 7Li, 11B in supernovae explosions ・νoscillations and possible restrictions on θ13 ● ν-16O reactions ● GT strength in Fe and Ni isotopes evaluated by a new Hamiltonian in fp-shell, GXPF1J ・ ν-56Fe reactions ・ν-56Ni reactions and synthesis of55Mn in starｓ

  4. 1. New Shell-Model Hamiltonians in p-shell and Neutrino-Nucleus Reactions p-shell（p-sd）　Cohen-Kurath+Millener-Kurath →SFO [ p: CK (8-16)2BME, p-sd: MK, sd, p2-(sd)2: Kuo’s G-matrix] Monopole terms in p1/2-p3/2 , T=0 enhanced：ΔV = -1.9 MeV SFO: Suzuki, Fujimoto, Otsuka, PR C67, 044302 (2003) Systematic improvements in the description of magnetic moments, GT transitions in p-shell nuclei are obtained.

  5. G-matrix vs phenom. interactions tensor force Shell evolution in N=8 isotone 6 8 Otsuka, Suzuki, Fujimoto, Grawe, Akaishi, PRL 69 (2005) Li Be B

  6. Magnetic moments of p-shell nuclei B(GT) for 12C →12N SFO present = SFOSuzuki, Fujimoto, Otsuka, PR C67 (2003) PR C55, 2078 (1997) Space: up to 2-3 hw SFO*: gAeff/gA=0.95 B(GT: 12C)_cal = experiment Suzuki, Chiba, Yoshida,Kajino, Otsuka, PR C74, 034307, (2006).

  7. ν-12C Exclusive 12C →12N (1+) Allen et al. (1990) EXP Exp: LSND PR C64 (2001) ●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*: gAeff/gA=0.95 Suzuki, Chiba, Yoshida, Kajino, Otsuka, PR C74 (2006)

  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= 0.65 (CK) Quenching of spin-dipole strength

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

  10. Cross sections for Supernova Neutrinos with temperature T Proton and neutron emissionsBR: Hauser-Feshbach model νSpectra

  11. Abundances of 7Li and 11B produced in supernova explosion processes M=16.2 M☼ (SN 1987A) No oscillation case Suzuki, Chiba, Yoshida, Kajino and Otsuka, PR C74, 034307 (2006)

  12. mix mix no mix mix no mix no mix 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 Increase by a factor of 2.5 and 1.4 7Be,11Cabundance Increase in the rates of charged-current reactions 4He(ne,e-p)3He and 12C(ne,e-p)11C in the He layer

  13. normal inverted no mix 7Li/11B Dependence on Mass Hierarchy and q13 N(7Li)/N(11B) Good indicator for neutrino oscillation parameters 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 angleq13. Neutrino experiments Constraining upper limitof q13

  14. Normal Inverted ν2m=νe ν3m=νe H-res ν2 ν3 ν2m ν1m ν2 ν1m ν1 ν3m ν3 ν1 L-res

  15. G vs. phemom. ・Modification of SFO for 16O Full inclusion of tensor force ・p-sd: tensor->p+r LS -> s+r+w ・sd: Kuo G-matrix T=1 monopole terms more repulsive → SFO-tls more repulsion than G in T=1 more attraction than G in T=0

  16. ●ν-induced reactions on 16O Spin-dipole strengths in 16O 17F

  17. T= temperature of supernova ν gAeff/gA=0.95 CRPA: Kolbe, Langanke & Vogel, PR D66 (2002) cf. Van Giai relativistic model

  18. T= temperature of supernova ν CRPA: Kolbe, Langanke & Vogel, PR D66 (2002)

  19. 2. Neutrino-Nucleus Reactions in fp-shell Nuclei New shell-model Hamiltonians in fp-shell: GXPF1:Honma et al., PR C65 (2002); C69 (2004) KB3: Caurier et al., Rev. Mod. Phys. 77, 427 (2005) ○KB3G A = 47-52 KB + monopole corrections ○ GXPF1 A = 47-66 ・ Systematic reproduction of E(2+) and B(E2) in fp-shell nuclei ・ Spin properties of fp-shell nuclei are well described ● GT Strengths in Ni and Fe Isotopes and M1 strengths in fp-shell nuclei

  20. M1 strength (GXPF1J) 8-12MeV 7-12MeV 7-12MeV 8-13MeV fp-shell B(GT) for 58Ni Honma gSeff/gS=0.75±0.2 Exp: Fujita et al. gAeff/gAfree=0.74

  21. B(GT+) GXPF1J EXP. 54Fe 4.0 3.3+/-0.5 56Fe 2.9 2.8+/-0.3 58Ni 4.7 3.8+/-0.4 60Ni 3.4 3.1+/-0.1 EXP: GT-; Rapaport et al., NP A410, 371 (1983) 0<Ex<13-15 MeV GT+; Caurier et al., NP A653, 439 (1999) 0<Ex<8 MeV

  22. GXPF1J Honma et al. cf. KB3 Caurier et al. KARMEN B(GT)=9.5 B(GT)exp=9.9±2.4 B(GT)KB3G=9.0 SD + … : RPA (SGII)

  23. GXPF1J 1+: shell-model 0-, 1-, 2- etc. : RPA gAeff/gAfree=0.74 Quenching of M2 strength in 48Ca and 90Zr gSeff=0.64gS P. von Neumann-Cosel et al., PRL 82, 1105 (1999)

  24. Neutral current reaction on 56Ni B(GT)=6.2 (5.4) GXPF1J (KB3G)

  25. Synthesis of Mn in Population III Star cf: HW02 gamma p n

  26. Synthesis of Mn in Population III Star Suzuki et al., PR C79 (2009) OBS: Cayrel et al., Astron. Astrophys. 416 (2004) No n GXPF1J HW02

  27. Production of 59Co Suzuki et al., PR C79 (2009) OBS: Cayrel et al., Astron. Astrophys. 416 (2004)

  28. Summary • Successful description of GT strengths in p-shell and fp-shell nuclei by new shell model Hamiltonians • Enhancement of ν-nucleus reaction cross sections: (ν, ν’p) • Enhancement of production yields of 7Li, 11B, and 55Mn in supernovae • Possible restriction on ν- oscillation parameters: θ13 , normal vs inverted

  29. Collaborators T. Yoshidab, S. Chibac, M. Honmad, K. Higashiyamae, H. Umedaf, K. Nomotof, D.H. Hartmanng, T. Kajinob,f and T. Otsukah bNational Astronomical Observatory of Japan cJapan Atomic Energy Agency dUniversity of Aizu eChiba Institute of Technology FDepartment of Astronomy, University of Tokyo gDept. Of Physics and Astronomy, Clemson University hDepartment of Physics and CNS, University of Tokyo

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

  31. neutron ESP

  32. ν-原子核反応 ・超新星ν Supernovae νSpectra Fermi-Dirac 分布 • DARν DAR ν spectra

  33. C1: 64% of TRK observed at Ex <30 MeV (Pywell et al.) cf. calc.～TRK at Ex <35 MeV E1: gv q=0.9～1.0 C1: q2= 0.7

  34. Yoshida, Umeda, Nomoto [Mn/Fe] No ν -0.53 HW02 -0.29 [Mn/Fe] GXPF1J(GT) -0.25 GXPF1J(all) -0.19 KB3G(GT) -0.3 No ν With ν(GXPF1J With ν(Woosley)

  35. Magnetic moments of p-shell nuclei B(GT) values for 12C -> 12N SFO B(GT) values for 14N -> 14C SFO present = SFO Suzuki, Fujimoto, Otsuka, PR C67 (2003) Space: up to 2-3 hw Negret et al., PRL 97 (2006) KVI RCNP SFO*: gAeff/gA=0.95 B(GT: 12C)_cal = experiment

  36. Magnetic moments of p-shell nuclei Energy levels of B isotopes Space: up to 2-3 hw present = SFO Suzuki, Fujimoto, Otsuka, PR C67 (2003) 10B g.s. 3+

  37. B(GT) values for 14N -> 14C B(GT) values for 12C -> 12N SFO SFO SFO*: gAeff/gA=0.95, B(GT: 12C)_cal = exp. KVI RCNP PR C55, 2078 (1997) Space: up to 2-3 hw Suzuki, Chiba, Yoshida,Kajino, Otsuka, PR C74, 034307, (2006). Negret et al., PRL 97 (2006)

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

  39. Cross sections for Supernova Neutrinos with temperature T Proton and neutron emissionsBR: Hauser-Feshbach model νSpectra

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

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