長寿命アイソマーと核構造超新星ニュートリノ過程

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1 新学術領域素核宇宙の融合第 2 回研究会クォーク力学原子核構造に基づく爆発的天体現象と元素合成 2010 年 5 月 31 日 ~6 月 1 日東京大学理学部天文教室長寿命アイソマーと核構造超新星ニュートリノ過程梶野敏貴 (NAO/UT) 吉田敬, 中村航, 茂山和俊, 野本憲一, 梅田秀之, 岩本信之 + H. 横枕 K. 木村 A. 高村 + 早川岳人鈴木俊夫大塚孝治 + D.H. Hartmann, G.J. Mathews M.K. Cheoun+

2 Neutrino Hamiltonian H tot = H ν + H νν H ν = Mixing and Interaction with Background Electrons p 1 ν e p 1 ν x MSW (Matter) Effect Mikeheev-Smirnov-Wolfebstein (1978, 1985) x N e = electron density H νν = Self-Interaction p 1 ν e p 2 ν e Exact solution, still UNKNOWN! p 2 ν x p 1 ν x

ν i + ν i e + + e - 2γ (Τ) ν µ ν τ νmasses Generation Key Physics suggested by FINITE mass neutrinos Unification of

3 ニュートリノの質量 Neutrino Masses 1 < 他の素粒子の質量 Quark & Lepton Masses 10,000,000,000 Quark & Lepton Masses E = mc 2 Why 10 ー 10? This could be a signature of new physics at times higher energy scale than the ordinary scale. ν i + ν i e + + e - 2γ (Τ) ν µ ν τ νmasses Generation Key Physics suggested by FINITE mass neutrinos Unification of forces in the early Universe? CP violation and Lepto-baryogenesis? Majorana or Dirac? Difference of mixing angles between q s and ν s?

4 Neutrino, Majorana or Dirac? Oscillation Mass Hierarchy! We have only ν L & ν R without ν R & ν L! Dirac mass term: Majorana mass term: Neutral particle m(ν L ) m(ν R ) Only light ν L exists, ν R be massive See-saw (Yanagida 1979) Special Relativity Helicity flip mass ν L ν R Germany-Japan Sep 29-Oct 2 Lepton number violation (Fukugita & Yanagida, PLB174 (1986), 45)

astro-particle physics method, unknown ν-oscillation

5 1.9K CMB Cosmic Background Neutrino Cosmology verification of particle model How to know/determine, in astro-particle physics method, unknown ν-oscillation parameters Σm ν, θ 13, and m 13 2 using SN ν-process nucleosynthesis!

Super-K, SNO, KamLand (reactor ν) determined m 12 2 and θ 12

6 Super-K, SNO, KamLand (reactor ν) determined m 12 2 and θ 12 uniquely. KNOWN Neutrinos Super Kamiokande (atmospheric ν) determined m 23 2 and θ 23 uniquely. + Cabbibo Angle m 12 2 m 23 2 LMS SN-neutrinos: Yokomakura et al. PL B544, 286 Θ 12 Several UNKNOWNs Θ 23 (1)sin 2 2θ 13 < 0.1, (2) m 132 = 2.4x10-3 ev 2 (3) δ=cp-phase, (4) Absolute Mass Yamazaki, Ichiki, Kajino, Mathews (2009,2010)

7 Solar System Abundance BIG-BANG Supernova-ν Process? STARS R-PROCESS SUPERNOVAE ELEMENTS UNKNOWN R-PROCESS SITES?? R S(N=50) S-PROCESS IN AGB STARS COSMIC-RAYS R S(N=82) R S(N=126) ++ + Actinide 232 Th (14.05Gy) P 238 U (4.47 Gy) Supernova-γ Process

8 New estimate for the time-dependent thermal nucleosynthesis of Ta180 m, T. Hayakawa, T. Kajino, S. Chiba, and G. J. Mathews, Phys. Rev. C81 (2010), 科学新聞 2010 年 5 月 28 日 ( 金 )

9 Type II Supernova ν-process & Several Key Nuclei MSW High-Density Resonance ν ν MSW (matter) Effect On Nucleosynthesis 180 Ta, 138 La, 92 Nb, 98 Tc, 26 Al

7 Li/ 11 B - Ratio 7 Li/ 11 B Normal Mass Hierarchy MSW Effect: Wolfenstein 1978, PR D17, 2369; Mikheyev & Smirnov 1986, Sov. J. Nucl. Phys. 42, 913. Yoshida, Kajino et al.

10 7 Li/ 11 B - Ratio 7 Li/ 11 B Normal Mass Hierarchy MSW Effect: Wolfenstein 1978, PR D17, 2369; Mikheyev & Smirnov 1986, Sov. J. Nucl. Phys. 42, 913. Yoshida, Kajino et al.,2005, PRL94, ; 2006, PRL 96, ; 2006, ApJ 649, 319; 2008 ApJ 686, 448. Astrophysics: Mass Hierarchy m Mixing Angle θ 13 No Mixing Inverted Long Baseline Exp: T2K (Kamioka) T2KK (KOREA) Double CHOOZ Daya Bay

11 Hamiltonian Dependence of ν-a cross section? Haxton s SM cal. (Woosley et al. ApJ. 356 (1990), 272) Suzuki s new SM cal. with NEW Hamiltonian Suzuki, Chiba, Yoshida, Kajino & Otsuka, PR C74 (2006), Suzuki, Fujimoto & Otsuka, PR C67, (2003) SFO 12 C: SFO Hamiltonian = Spin-isospin flip int. with tensor force to explain neutron-rich exotic nuclei. - µ-moments of p-shell nuclei - GT strength for 12 C 12 N, 14 C 14 N, etc. (GT) - DAR (ν,ν ), (ν,e-) cross sections Cheoun et al., PRC81 (2010), : QRPA SFO 12 C(ν e,e - ) 12 N 12 C(ν e,e - ) 12 N(gs,1 + ) GT

12 Haxton s SM cal. (Woosley et al. ApJ. 356 (1990), 272) Suzuki s new SM cal. with NEW Hamiltonian Suzuki, Chiba, Yoshida, Kajino & Otsuka, PR C74 (2006), Otsuka, Suzuki, Fujimoto, Grawe, Akaishi, PRL 69 (2005). 4 He: WBP Hamiltonian = Warburton & Brown, PRC 46 (1992), 923. = Similar result to microscopic ab initio calculation of Gazit et al. PRC70 (2004) He 4 He(ν, ν ) 4 He* WBP

13 No ν-beam experiment yet for ν-a X-section! We can use Electro-Magnetic PROBE! Similarity between Electro-Magnetic & Weak Interactions EM-current = V, Weak-current = V - A IV i gv V gv σ q+ ( p+ p') 2m 2m A g σ A Weak operator in non-relativistic limit Gamow-Tellar operator = Spin-Dipole operator = 4 He(γ, n) 3 He and 4 He(γ, p) 3 H σ τ ± J [ σ r ] τ ± Big-Bang nucleosynthesis with SUSY particle 4 He(ν, ν ), 4 He(ν e, e - ), 4 He(ν e, e + ) SN-ν nucleosynthesis for determining ν-oscillation param

New SM-σ ν (E) using WBP( 4 He) & SFO( 12 C) interactions Suzuki, Chiba, Yoshida, Kajino & Otsuka, Phys.

14 Hamiltonian Dependence of MSW-Effect on 7 Li/ 11 B Previous SM-σ ν (E) of Haxton Woosley, Haxton, Hoffmann, Wilson, ApJ. (1990). Hoffmann & Woosley, ApJ. (1992). New SM-σ ν (E) using WBP( 4 He) & SFO( 12 C) interactions Suzuki, Chiba, Yoshida, Kajino & Otsuka, Phys. Review C74 (2006), normal Normal 0.6 inverted Inverted Normal / inverted, well separated! 7 Li/ 11 B-ratio is SM independent! Mixing angle θ 13 dependence, almost the same!

Laser Compton-scattered photon (LCS-γ) Klein

15 Laser Compton-scattered photon (LCS-γ) Klein Nishina formula E γ 2 4hc γ =, γ = 2 2 λ 1+ γ θ L E m c e 2 e Relativistic electron (E e ) Laser light (λ L ) Yoshio Nishina γ (E γ ) Spring-8 E γ (θ) θ λ L =1.064µm, E e =800MeV E γ = 11MeV λ L =1.064µm, E e =1.5GeV E γ = 39MeV New Subaru Prof. Miyamoto

16 Gamow-Teller (β-decay) Strength Distribution in 55 Mn- 56 Fe- 56,58 Ni region Suzuki, Honma, Higashiyama, Yoshida, Kajino, Otsuka, Umeda & Nomoto, PRC79 (2009), (R). Experiment: Rapaport (1983), NP A410, 371. Exp. Shell Model Cal. Previous SM Cal.

17 Uncertainties in Neutrino-Spectrum? T(ν e ) = 3.2 MeV < T(ν e ) = 5.0 MeV < T(ν µ,τ ) = T(ν µ,τ ) = 6.0 MeV ε(ε ν ) / ε Neutrino energy distr ibution e e,,, - SN1987A Neutrinos? Only 11 ν-events, too small, but total Energy is estimated! - Nucleosynthetic Calibration Galactic Chemical Evolution of the Light LiBeB Elements, ε ν (MeV) Meteoritic 11 B/ 10 B-Ratio.

Grav. Potential constraint Detection of Direct Supernova νs Yoshida, T., Kajino, T., and Hartmann, D., PRL 94 (2005), 231101. Consistent with SN1987A!

18 Grav. Potential constraint Detection of Direct Supernova νs Yoshida, T., Kajino, T., and Hartmann, D., PRL 94 (2005), Consistent with SN1987A! Woosley & Weaver ApJS 101 (1995), 181. OVERPRODUCTION Various progenitor mases Consistent with Thomas-Janka et al (MPA) GCE constraints on 11 B from meteoritic 11 B/ 10 B Yoshida-Kajino-Hartmann (2005)

19 Galactic Chemical Evolution of 9 Be & 10,11 B Overproduction Livermore Model Tν µ,τ = 8 MeV Woosley & Weaver 1995 ApJS 101, 181. Tν µ,τ = 6 MeV Yoshida, Kajino & Hartmann 2005, PRL 94 (2005), OLD stars SUN 9 Be, produced by: -Galactic Cosmic Rays B, produced by: -Supernova ν process -Galactic Cosmic Rays

20 科学新聞 2010 年 5 月 28 日 ( 金 )

21 Origin of 180 Ta & 138 La 138 La ~ spherical nucleus 180 Ta ~ deformed nucleus K.Yokoi, Nature (1983) Proposal of s-process origin D.Belic et al., Phys. Rev. Lett. (1999) Measurement of transition probability between the isomer and the ground states K.Wisshak, Phys. Rev. Lett. (2001) Neutron capture cross section of 180Ta 1.82y 179 Ta Neutral current Goko, Phys. Rev. Lett. (2007) Measurement of (gamma,n) reactions D. Byelilov, Phys. Rev. Lett. (2007) (3He,t) experiments for neutrino-process GT, measured at RCNP: E n < 50 MeV! M.-K.Cheoun et al., (2010), in preparation. Supernova neutrino-process: Woosley, Hartmann, Hoffman, & Haxton, ApJ 356 (1990), 272. Heger et al., Phys. Lett. B 606, 258 (2005) Nucleo-Cosmochronology: Hayakawa, Shimizu, Kajino, Ogawa, & Nakada, PRC 77 (2008), ; 79 (2009)

22 Supernova ν-process of 138 La A. Heger, Phys. Lett. B 606, 258 (2005) Charged Current Neutral Current γ-process ~ 10 9 K Neutrino-process ~ 10 8~9 K

23 Effect of Charged Current reaction Byelikov + Fujita et al., PRL (2007) A. Heger, recalculated Supernova measured GT strength at RCNP, Osaka. nucleosynthesis of 138 La & 180 Ta La 180Ta solar gamma only nc 6MeV cc 4MeV cc 6MeV cc 8MeV Overproduction Problem of 180 Ta relative to 138 La! Spin-dipole and multipole forbidden transitions + GT does!

24 Problem of Isomer Ratio Isomer Residual Ratio, isomer / (gs+isomer), is a critical factor for calculation of 180Ta nucleosynthesis. Linking transitions between K = 1 and K = 9 bands are extremely weak. Theoretical formula for Al26 with strong linking transitions does not apply! Excitatoin Energy Photons Planck Distribution Photon Flux 180 Ta g and 180 Ta m couple with each other through intermediate linking transitions. K = Ta0 180 Ta g Intermediate states K = 9 T 1/2 =8.15 h Isomer 180 Ta m Intermediate states T 1/2 > y

26 In general cases: Formula to calculate time-dependent linking transitions Hayakawa, Kajino, Chiba & Mathews, PR C81 (2010) In the case of 180 Ta: Transition probabilities Experimental Data

28 Measured Widths D. Belic et al., PR C65 (2002),

29 Nuclear Structure of 180 Ta Excited states in 180 Ta have been studied well by using in-beam gamma-ray spectroscopy. T.R. Saitoh, NPA 1999, NBI group G. D. Dracoulis, PRC 1998, ANU group

30 Calculated Result Hayakawa, Kajino, Chiba & Mathews, PR C81 (2010), Isomer Ratio Pi = 0.39 Present linking dynamical cal. Hayakawa et Sudden al. (2009) Freeze Out Critical Temperature Mohr, 2007 We carried out timedependent dynamical calculations. Model: T = exp( -t /τ) τ = 0.3, 1, 3 s 0.1 Freeze-Out Region Transitional Region Thermal Equilibrium Region Init : T9 = Temperature (10 9 K)

31 New Result La 180Ta 180Ta isomer We multiply the calculated abundance by the factor of Pi = Both the nuclei can be reproduced consistently by +CC at 4MeV. 0 solar gamma only nc 6MeV cc 4MeV cc 6MeV cc 8MeV Heger, PLA, 2005 Byelikov, PRL, 2007

32 Neutrino Hamiltonian H tot = H ν + H νν H ν = Mixing and Interaction with Background Electrons p 1 ν e p 1 ν x MSW (Matter) Effect Mikeheev-Smirnov-Wolfebstein (1978, 1985) x N e = electron density H νν = Self-Interaction p 1 ν e p 2 ν e Exact solution, still UNKNOWN! p 2 ν x p 1 ν x

Lisi, A. Marrone, & A. Mirizzi, JCAP 12, (2007) 010. A. B.

33 ν self-interaction (Quantum Effect) ν-sphere in SN core H. Duan, G.M. Fuller, J. Carlson, Y.-Z. Qian, PRL 97 (2006), G. Fogli, E. Lisi, A. Marrone, & A. Mirizzi, JCAP 12, (2007) 010. A. B. Balantekin, Y. Pehlivan, J. Phys.G34, (2007) 47. r = 200km Swapping! High-energy

34 SUMMARY The n-process in core-collapse SNe provides unique tool in terms of MSW effect to determine the unknown ν-oscillation parameter θ 13 and mass hierarchy of active ν s. Neutrino-Nuclear Astrophysics takes the keys to elucidate Cosmic, Galactic and Stellar Evolution in terms of nucleosynthesis. Time is matured to promote US-Japan Collaboration in this field to: - provide fundamental knowledge of neutrino-nucleus interactions, - apply to nucleosynthesis & evolution of various stellar objects. US-Japan Nucl. Astro. THEORY: Discussion has just launched. Extension of JUSTIPEN; UT- IPMU; 10 peta flops Supercomputer in particle-nuclear-astrophysics unification in Japan Nucl. EXPERIMENT: Promissing!? ORNL-JPARC (in Neutrino Beam Physics) FRIB (MSU)-RIBF (RIKEN) (in Exotic Nuclear Physics) Astronomy & Particle Astrophys.: Will go!? 30 Meter Telescope (TMT); Hyper-Kamiokande

35 Hamiltonian Dependence of MSW-Effect on 7 Li, 11 B Yoshida, Suzuki, Chiba, Kajino, Yokomakura, Kimura, Takamura & Hartmann, ApJ 686 (2008), 448. PSDMK: OXBASH: Brown, Etchegoyen & Rae, MSU-CL Report No. 524 (1986); Millener & Kurath, NPA 255 (1975), 315. WBP: Warburton & Brown, PRC 46 (1992), 923, SFO: Suzuki, Fujimoto & Otsuka, PR C67, (2003), HW92: Hoffman & Woosley, LLNL-HP (1992); Woosley, Hartmann, Hoffman & Haxton, ApJ 356 (1990), 272. Absolute 7 Li & 11 B yields depend strongly on different Hmiltonians! But, MSW effect is quantitatively very similar to one another!

原子核の弱電相互作用と超新星ニュートリノ

京都大学物理学第二教室談話会 2010 年 10 月 15 日原子核の弱電相互作用と超新星ニュートリノニュートリノ温度および振動パラメータの決定方法の提案梶野敏貴国立天文台理論研究部東京大学大学院理学系研究科天文学専攻 Neutrino Physics and Cosmology Today Neutrino Mass Cosmology CMB and LSS constraint from

長寿命アイソマーと核構造 超新星ニュートリノ過程

長寿命アイソマーと核構造超新星ニュートリノ過程