Supernova Ncleosynthesis and Neutrino Oscillation

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1 10 th Russbach School on Nuclear Astrophysics Salzburg, Austria, March 10-16, 2013 Supernova Ncleosynthesis and Neutrino Oscillation θ 13 is known! Mass hierarchy and CP-pahse come next? Taka KAJINO National Astronomical Observatory Department of Astronomy, University of Tokyo

What is the Cold Dark Matter, W CDM = 0.23, and Dark Energy, W L = 0.73? CMB including n-mass: Yamazaki, Kajino, Mathews & Ichiki, Phys. Rep. 517 (2012),141-167. Is BARYON sector, W B = 0.

2 What is the Cold Dark Matter, W CDM = 0.23, and Dark Energy, W L = 0.73? CMB including n-mass: Yamazaki, Kajino, Mathews & Ichiki, Phys. Rep. 517 (2012), Is BARYON sector, W B = 0.04, well understood? Challenge of the Century Universal expansion is most likely accelerating and flat! BBN with Axions + SUSY to solve Dark Matter Problem & Li Problem: Kusakabe, Balantekin, Kajino & Pehlivan, Phys. Lett. B718 (2013) 704. SUSY-DM m n = 0 is the unique signal to go beyond the Standard Model! n mass and hierarchy? Today s Talk W B + W CDM + W L = 1 Supernova n-process Nucleosynthesis to determine the n-mass HIERARCHY.

3 Higgs(standard model) produces Quark Masses. Neutrino Masses 1 = Quark & Lepton Masses 10,000,000,000 E = mc 2 Why 10-10? This could be a signature of new physics at times higher energy scale than the ordinary scale. n i + n i e + + e - 2g (T)? n ν-masses require a theory beyond the standard model! Generation n Key Physics suggested by FINITE mass neutrinos: Unification of elementary forces beyond the standard model? CP violation and Lepto- & Baryo-genesis? Why left-handed neutrinos, Majorana or Dirac? Explosion Mechanism of Supernovae?

KNOWN of Neutrino Oscillations KAMIOKANDE, SK, KamLand (reactor ν), SNO determined m 12 2 and θ 12 uniquely, and also SK (atmospheric ν) determined m 23 2 and θ 23 uniquely. 23-mixing sin 2 2q 23 = 1.

4 KNOWN of Neutrino Oscillations KAMIOKANDE, SK, KamLand (reactor ν), SNO determined m 12 2 and θ 12 uniquely, and also SK (atmospheric ν) determined m 23 2 and θ 23 uniquely. 23-mixing sin 2 2q 23 = 1.0 Δm 2 23 = ev 2 12-mixing sin 2 2q 12 = (q 12 +q C =p/2) Δm 2 12 = ev 2 Cabibbo angle UNKNOWN 13-mixing, hierarchy, CP, mass sin 2 2q 13 (< 0.1) T2K, MINOS, RENO, Daya Bay, Double Chooz m 2 13 = ±2.4x10-3 ev 2 δ=cp violation phase Absolute Mass 0nbb, cosmology E(n )=E(n ): Yokomakura et al., PL B544, 286.

5 1.9K Various Neutrino-Sources in Nature CMB Cosmic Background Neutrino Cosmology verification of particle model n e, n, n n e, n, n SN n-spectra are still unknown!

6 Number Abundance (Si = 10 6 ) Solar System Abundance Big-Bang Nucleosynthesis 1,2 H, 3,4 He, 6,7 Li, etc. Stellar Fusion 12 C 56 Fe- 58 Ni, etc. (r-nuclei) (s-nuclei) Core-Collapse SNe & AGB: 56 Fe < A Iron peak Supernova n-nucleosynthesis Li-Be-B r-nuclei np-nuclei p-nuclei 92 Nb 98 Tc 138 La 180 Ta 232 Th (14.05Gy) 238 U (4.47 Gy) Cosmic Ray Spallation Li-Be-B, F, Na, etc. Mass Number A

Various roles of n s in SN-nucleosynthesis 8 8 MSW resonance at r~10 3 (g/cm 3 ) n-flavor Oscillation n-n Scattering near Proto-Neutron n-collective Flavor Oscillation n n e

7 Various roles of n s in SN-nucleosynthesis 8 8 MSW resonance at r~10 3 (g/cm 3 ) n-flavor Oscillation n-n Scattering near Proto-Neutron n-collective Flavor Oscillation n n e NS Si Layer R-process: Heavy Nuclei np-process: 92 Mo, 96 Ru? Explo. Si-burn. Fe-Co-Ni, 60 Co, 55 Mn, 51 V n-process 180 Ta, 138 La, 92 Nb, 98 Tc n-process: 6,7 Li, 9 Be, 10,11 B

8 Proton Number Z Supernova Nucleosynthesis Simulation Chiba, Koura, Kajino n-pair Heated Collapsar Model K. Nakamura, et al. ApJ (2013). 235 U 208 Pb Fe Neutron Number N

9 R-process Nucleosynthesis Otsuki, Tagoshi, Kajino and Wanajo, ApJ 533 (2000), 424; Wanajo, Kajino, Mathews and Otsuki, ApJ J. 554 (2001), 578. Neutron-rich condition for successful r-process: 0.1 < Y e < 0.48 n e + n p + e - n e + p n + e + -1 Theoretical Challenge: en = 3.15 Tn T ne = 3.2 MeV, T ne = 4 MeV 1)Astrophysical Sites? n-wind SNe MHD jet SNe NS mergers GRBs Sr-Y-Zr I-Xe Theoretical model Ir-Pt 2)Neutrino effects? Pb Y e > 0.5? Roberts, Reddy and Shen (PR C86, , 2012) pointed out Dy-Er Y e < 0.5! for nucleon potential and Pauli blocking effects. Observed Solar r-abundance A

SN n-process overproduces 180 Ta! p process Burbidge 2 -Fowler-Hoyle, Rev. Mod. Phys.

10 Tantalum( 180,181 Ta) 181 Ta g (stable), 180 Ta g (unstable, 1/2 = 8h), 180 Ta m (isomer, 1/2 > y) The rarest isotope in the Universe! Origin of 180 Ta was unknown. SN n-process overproduces 180 Ta! p process Burbidge 2 -Fowler-Hoyle, Rev. Mod. Phys. 29 (1957), Element Genesis Neutral current (n e ) in Supernovae r process (1990) J. Burbidge M. Burbidge W. Fowler F. Hoyle

11 Supernova n-process Nucleosynthesis A. Heger, Phys. Lett. B 606, 258 (2005) La 180Ta solar system gamma only nc 6MeV cc 4MeV cc 6MeV cc 8MeV T ne Byelikov + Fujita et al., PRL (2007), RCNP measurement of GT strength. Overproduction of 180 Ta relative to 138 La!

12 Excitatoin Energy 180 Ta-genesis needs Quantum Phys. + SN Hydro-dyn. Solar- 180 Ta is all ISOMER with T 1/2 > y! Long lived 180 Ta m is excited to intermediate states in the photon bath in SNe, and decay with the ground state in 8 hours. We solved dynamical explosive SN-nucleosynthesis coupled with quantum transitions simultaneously. (Hayakawa, et al. 2010, PR C81, ; PR C82, ) Photons Planckian Distribution Distribution Intermediate States states Intermediate states Photon Flux K K=1 = Ta Ta g spherical G.S. K=9 K = 9 T 1/2 =8.15 h b decay T 1/2 = 8.15h Isomer 180 Ta m T 1/2 > y Isomer - deformed T 1/2 > y

13 n-process and Structure of 180 Ta Saitoh et al. (NBI group), NPA 1999, + Dracoulis et al. (ANU group), PRC 1998, + J = Total Quantum Number Linking transitions between K = 1 and 9 bands are extremely weak. K=9 K Quantum Number K=1 D. Belic et al., PR C65 (2002), g i /g 0 G i G 0 /G tot gr. state 1 + isomer 9 - Excitation Energy [MeV]

14 Formula to calculate time-dept linking transitions Hayakawa, Kajino, Mohr, Chiba & Mathews, PR C81 (2010), ; PR C82 (2010), General formula (Einstein AB theory) for kt << ΔE ij : P p q q p p In the SPECIFIC case of 180 Ta: Transition prob. S p A ip = G i / h Exp

15 Result from n-nucleosynthesis 138La 138La 138La 180Ta 180Ta 180Ta 180Ta isomer 180Ta Heger et al. PLB606, 258 (2005) (Overproduction) (Our new result) T. Hayakawa, T. Kajino, S. Chiba, and G.J. Mathews, Phys. Rev. C81 (2010), About 40% 180 Ta m survives in supernova explosion. Then, both 138 La and 180 Ta abundances can be consistently reproduced by the CC-int. of n e and n e of T ne = T ne = 4 MeV. 1 1 Consistent with r-process! 0 0 solar system gamma gamma only only nc 6MeV cc 4MeV cc 6MeV cc 8MeV nc 6MeV cc 4MeV cc 6MeV cc 8MeV T ne = 3.2 MeV, T ne = 4 MeV.

Supernova n-process to estimate Tn, and Tn SN II: Yoshida, Kajino & Hartman, Phys. Rev. Lett. 94 (2005), 231101.

16 Supernova n-process to estimate Tn, and Tn SN II: Yoshida, Kajino & Hartman, Phys. Rev. Lett. 94 (2005), SNIc + II: Nakamura, Yoshida, Shigeyama, Kajino, ApJL 718 (2010), L137. n Abundance X A n ~85% ~15% Suzuki, Chiba, Yoshida, Kajino & Otsuka, PRC74 (2006),

17 Overproduction Problem of Supernova- 11 B S. M. Austin, Prog. Part. Nucl. Phys. 7, 1 (1981) - Meteoritic Abundances: 11 B/ 10 B = (GCR + SNe) - Galactic Cosmic-Ray: 11 B/ 10 B = (GCR) SUPERNOVA Nucleosynthesis: Hoffman, Woosley & Weaver 2001, ApJ 549, B: Overproduced! 10 B:Normal!

18 Galactic Chemical Evolution of 9 Be & 10,11 B Livermore Model Tn, = 8 MeV Woosley -Weaver 1995, ApJS 101, 181. s E n 2 Tn, = 6 MeV Consistent with SN1987A Overproduction problem is resolved! Yoshida, Kajino & Hartmann 2005, PRL 94 (2005), OLD stars SUN 9 Be: -Galactic Cosmic Rays B + 11 B: -Galactic Cosmic Rays -Supernova n-process Yoshii, Kajino, Ryan, 1997, ApJ 486, 605. Ryan, Kajino, Suzuki, 2001, ApJ549, 55.

19 SN1987A constraint on E n,tot & Grav. Energy SN-Boron calculations and constraints on SN- n Woosley & Weaver ApJS 101 (1995), 181. T n = 8 MeV T n = 6 MeV Yoshida, Kajino & Hartman, Phys. Rev. Lett. 94 (2005), Consistent with SN simulation (MPA group) GCE constraints on 11 B & meteoritic 11 B/ 10 B

GCE of Light Elements & 11 B Tn, = Tn = 6 MeV 0.25 0.2 0.15 0.1 0.

20 e(e n ) / e Average n-temperatures are now known! R-process Elements & 180 Ta/ 138 La Tn e = 3.2 MeV, Tn e = 4 MeV Astron. GCE of Light Elements & 11 B Tn, = Tn = 6 MeV Neutrino Oscillation! n e T(n e ) < T(n e ) < T(n x ) n e MeV n,,n, e n (MeV)

21 Neutrino Oscillation (MSW Effect) through propagation n e spectrum Low-E comp. disappears! High-E comp. appears!, e Center E n outside Parameters: 25M solar progenitor SN model (Hashimoto & Nomoto 1999) - sin 2 2q 13 = m 13 2 = 2.4x10-3 ev 2 - L n = 3x10 53 erg, n = 3 sec - T ne =3.2MeV, T ne =5.0MeV, T n =6.0MeV E n

22 7 Li and 11 B are produced in the He/C Shell [ ] MSW high-density resonance is located at the bottom of C shell. n x n e n x n e

23 larger effect! Yoshida, Kajino, Yokomakura, Kimura,Takamura & Hartmann, PRL 96 (2006) 09110; ApJ 649 (2006), 349. T ne < T ne < T n, n smaller effect! Normal L H-Resonance m n L Normal Mass Hierarchy N e Inverted Inverted m n H-Resonance NO 13-mixing N e

24 Bayesian Analysis, including astrophysical model dependence on SN progenitor mass, n-temp. ( T ne,t ne,t n, n ) and nuclear input data. SN progenitor Mass aa(a,g) 12 C 12 C(a,g) 16 O

25 MSW Effect & n Mass Hierarchy Normal Mass Hierarchy Yoshida, Kajino et al. 2005, PRL94, ; 2006,PRL 96, ; 2006, ApJ 649, 319; 2008, ApJ 686, Li/ 11 B-Ratio Inverted Mass Hierarchy Long BaselineExp. in 2011: T2K (Kamioka) MINOS Reactor Exp. in2012: Double CHOOZ Daya Bay RENO (KOREA) sin 2 2q 13 =

2 2q 23 =1 Minos (2011) T2K (2012) q 13 Reactor n RENO, Daya

26 Long Baseline n T2K & MINOS (2011) Normal sin 2 2q 13 = 0.1 Inverted Daya Bay 2012 Rino (2012) Double Chooz (2012) Sin 2 2q 23 =1 Minos (2011) T2K (2012) q 13 Reactor n RENO, Daya Bay & Double Chooz (2012) m 2 13 m 2 23 detector 1 detector 2

1/2 =60yr) SiC X-grains are made of Supernova Dust!

27 Murchison Meteorite SiC X-grains - 12 C/ 13 C > Solar - 14 N/ 15 N < Solar - Enhanced 28 Si - Decay of 26 Al (t 1/2 =7x10 5 yr), 44 Ti (t 1/2 =60yr) SiC X-grains are made of Supernova Dust! Fujiya, Hoppe and Ott (2011, ApJ 730, L7) discovered 11 B and 7 Li isotopes in 13 SiC X-grains.

1 0.9 Supernova X-Grain Coinstraint Normal Mass Hierarchy Mathews, Kajino, Aoki And Fujiya, Phys. Rev. D85,105023 (2012). 7 Li/ 11 B-Ratio 0.8 0.7 0.6 0.5 0.

28 1 0.9 Supernova X-Grain Coinstraint Normal Mass Hierarchy Mathews, Kajino, Aoki And Fujiya, Phys. Rev. D85, (2012). 7 Li/ 11 B-Ratio Inverted Mass Hierarchy T2K, MINOS (2011) Double CHOOZ, Daya Bay, RENO (2012) sin 2 2q 13 = 0.1 First Detection of 7 Li/ 11 B in SN-grains Inverted Mass Hierarchy is statistically more preferred! 74% ー Inverted 24% ー Normal W. Fujiya, P. Hoppe, & U. Ott, ApJ 730, L7 (2011)

7 Li/ 6 Li isotopic ratio has recently detected in supernova remnant IC443. (Ritchey et al.

29 More Observational Effort is required! Astron. Observations SN-remnants & r-enhanced metal-poor stars are enriched by SN-products! 7 Li & 11 B, separately detected! 7 Li/ 6 Li isotopic ratio has recently detected in supernova remnant IC443. (Ritchey et al. 2012) Presolar SiC grains X-grains are made of SN-dusts! P. Hoppe et al. ApJ 551 (2001) 478, W. Fujiya, P. Hoppe, and U. Ott, ApJ 730, L7 (2011). 7 Li/ 11 B; more data, required! Simultaneous detection is highly desirable!

30 n-nucleus Cross-Sections New Shell Model cal. with NEW Hamiltonian: n - 12 C, 4 He Suzuki, Chiba, Yoshida, Kajino & Otsuka, PR C74 (2006), Suzuki, Fujimoto & Otsuka, PR C67, (2003) 12 C: New Hamiltonian = Spin-isospin flip int. with tensor force to explain neutron-rich exotic nuclei. - -moments of p-shell nuclei - GT strength for 12 C 12 N, 14 C 14 N, etc. (GT) - DAR (n,n ), (n,e-) cross sections QRPA cal.: n Ta, 138 La, 98 Tc, 92 Nb, 42 Ca, 12 C, 4 He Cheoun, et al., PRC81 (2010), ; PRC82 (2010), : J. Phys. G37 (2010), ; PRC 83 (2011), Ta(n, n n ) 180 Ta 12 C(n e,e - ) 12 N GT Spin-Mutipole 12 C(n e,e - ) 12 N(gs,1 + ) GT Spin-Multipole

31 Hamiltonian Dependence on MSW-Effect Previous SM-s n (E) of Haxton Woosley, Haxton, Hoffmann, Wilson, ApJ. (1990). Hoffmann & Woosley, ApJ. (1992). New SM-s n (E) using WBP( 4 He) & SFO( 12 C) interactions Suzuki, Chiba, Yoshida, Kajino & Otsuka, PR C74 (2006), : Suzuki & Kajino, J. Phys. G (2013). 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!

Counts n-beam experiment is not available! EM-PROBE (CEX hadrons, g s)! Similarity between Electro-Magnetic & Weak Interactions 58 Ni( 3 He, t) 58 Cu E = 140 MeV/u Y. Fujita et al.

32 Counts n-beam experiment is not available! EM-PROBE (CEX hadrons, g s)! Similarity between Electro-Magnetic & Weak Interactions 58 Ni( 3 He, t) 58 Cu E = 140 MeV/u Y. Fujita et al., EPJ A 13 ( 02) 411. Y. Fujita et al., PRC 75 ( 07) 58 Ni(p, n) 58 Cu E p = 160 MeV J. Rapaport et al., NPA ( 83) EM-current = V, Weak-current = V - A IV i gv V gv s q ( p p') 2m 2m A g A s Weak operator in non-relativistic limit Gamow-Tellar operator = Spin-Multipole operator = s J J [ [ s r Y r (L) ] ] Excitation Energy (MeV)

Neutrino Hamiltonian: H tot = H n + H nn H n = Mixing and Interaction with Background Electrons MSW (Matter) Effect: Mikeheev-Smirnov-Wolfebstein (1978, 1985) p 1 n e p 1 n x H nn = Self-Interaction

33 Neutrino Hamiltonian: H tot = H n + H nn H n = Mixing and Interaction with Background Electrons MSW (Matter) Effect: Mikeheev-Smirnov-Wolfebstein (1978, 1985) p 1 n e p 1 n x H nn = Self-Interaction Self-Interaction x N e = electron density p 1 n e p 2 n e Quest for EXACT Many-Body SOLUTION! Invariants of collective neutrino oscillations Y. Pehlivan, A.B. Balantekin, T. Kajino & T. Yoshida Phys. Rev. D84, (2011) p 2 n x p 1 n x

34 n self-interaction (Quantum Effect) neutrino-phere 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

n-asymmetry under the Strong Dipole (Poroidal) Magnetic Field Fundamental Interactions among Hadrons (p, n, L, S ) and Lepton (e,n ) at High-r and High-T in Relativistic Field Theory and QCD

35 n-asymmetry under the Strong Dipole (Poroidal) Magnetic Field Fundamental Interactions among Hadrons (p, n, L, S ) and Lepton (e,n ) at High-r and High-T in Relativistic Field Theory and QCD Proto-neutron stars in c.c. Supernovae Maruyama, Kajino, Yasutake, Cheoun, & Ryu, PRD83 (2011), (R). L Neutrino scattering and absorption process inside the magnetized Neutron star (10 15 G) is asymmetric. ~ 2 % asymmetric n-abs. (drift) Enough for Pulsar-Kick By ~500km/s D.Page!

Why Amino Acids on the Earth, All Left-Handed? Chitrality, earth origin or universal? Neutrinos are all left-handed!

SN ejecta including 14 N interact with neutrino under strong magnetic field!

Boyd, Kajino, & Onaka suggested that the L-handed chirality of amino acids is UNIVERSAL! (Astrobio. 10, 2010, 561-568; Int. J.

36 Why Amino Acids on the Earth, All Left-Handed? Chitrality, earth origin or universal? Neutrinos are all left-handed! Supernovae with strongly magnetized neutron star or BH emit intensive flux of neutrinos over yrs! SN ejecta including 14 N interact with neutrino under strong magnetic field! Neutrino- 14 N coupling is asymmetric & chiral selective! Boyd, Kajino, & Onaka suggested that the L-handed chirality of amino acids is UNIVERSAL! (Astrobio. 10, 2010, ; Int. J. Mol. Sci. 12, 2011, 3432) Magnetized Supernovae 14 N lives! % 99.3% m e c 2 14 O ν e + 14 N e O 0.61% 14 N dies! Mann and Primakoff (Origins of Life, 11 (1981), 255) suggested β-decay of 14C, but it s too SLOW! ν e + 14 N e C C (5730y) 100% N (1+)

n-mass hierarchy: SUMMARY - We proposed a new nucleosynthetic method to estimate average n-spectra from core-collapse supernovae: T(n e ) = 3.2MeV, T(n e ) = 4.0MeV,

37 n-mass hierarchy: SUMMARY - We proposed a new nucleosynthetic method to estimate average n-spectra from core-collapse supernovae: T(n e ) = 3.2MeV, T(n e ) = 4.0MeV, T(n x ) = 6.0MeV. - 7 Li/ 11 B isotopic ratios of SiC X-grains (SN-grains) enriched in n- process materials have the potential to solve the mass hierarchy for finite q 13. Inverted hierarchy is more preferred statistically. Total n-mass: - Curvature perturbation is shown to be generated by the extra anisotropic stress π ext without tuning the initial condition of inflation-driven (pre-big-bang) perturbation. This would constrain the generation epoch and the nature of primordial (unknown) π ext. - Total n-mass is constrained to be S m ν < 0.2 ev from the MCMC analysis of CMB temperature and polarization anisotropies including the primordial magnetic field.

Nucleosynthesis in Supernovae and GRBs and Neutrino Oscillation

Meeting on Unification of Particle Physics, Nuclear Physics and Astrophysics, Ise-Shima, December 3-5, 2011 Nucleosynthesis in Supernovae and GRBs and Neutrino Oscillation Taka KAJINO National Astronomical