Crossover between Nuclear Physics & Astrophysics

Transcription

1 RCNP-KU Meeting on Crossover between Hadron Physics and Nuclear Physics September 4-6, 2013 Crossover between Nuclear Physics & Astrophysics Link among Cosmology-Neutrino-Supernovae-Nuclei Taka KAJINO COSNAP (= Cosmology & Nuclear Astrophysics Group) National Astronomical Observatory Department of Astronomy, The University of Tokyo

2 Nobu Yahiro jointed in my COSNAP collaboration since Our Joint Papers on COSMOLOGY, written together with/by him. N. Yahiro, G. J. Mathews, K. Ichiki, T. Kajino, and M. Orito, Phys. Rev. D65 (2002), , Constraints on Cosmic Quintessence and quintessential inflation. A model for Dark Energy K. Ichiki, M. Yahiro, T. Kajino, M. Orito, and G. J. Mathews, Phys. Rev. D66 (2002), , Observational constraints on dark radiation in brane cosmology. Extra-Dimension Brane Cosmology K. Ichiki, P. M. Garnavich, T. Kajino, G. J. Mathews, and M. Yahiro, Phys. Rev. D68 (2003), , Disappearing dark matter in brane world cosmology: New limits Extra-Dimension on noncompact extra dimensions. Brane Cosmology K. Umezu, K. Ichiki, T. Kajino, G. J. Mathews, R. Nakamura, and M. Yahiro, Phys. Rev. D73 (2006), , Observational Constraints on Accelerating Brane Cosmology A model for accelerating with Exchange between the Bulk and Brane International Conference Papers + Many Discussions on Nuclear Astrophysics cosmic expansion with L = 0 My/Our student, Kiyotomo Ichiki, was awarded President s Prize of the University of Tokyo!

3 Challenge of the Century Universal expansion is most likely accelerating and flat! W B + W CDM + W L = 1 CMB Planck What is CDM (W CDM = 0.27) and DE (W L = 0.68)? CMB including n-mass SN Ia magnitude-redshift relation Is BARYON sector (W B = 0.05) well understood? BBN with Axions + SUSY to solve DM & Li Problems: SUSY-DM beyond the Standard Model m n = 0 is the unique signal! The 1st Purpose :- is to clarify the scintific link among Big-Bang Nucleosynthesis Dark Matter & Neutrino Mass Non-thermal & Thermal (CMB) Photons.

4 Plateau like HIGH 6,7 Li ABUNDANCE --- primordial? Abundance scatter is too small to accept DEPLETION of factor 3!? 7 Li BBN T = 1~3x10 6 K 7 Li(p,a) 4 He BBN prediction ~ > 3 Cosmological? Observed 7 Li Solar 7 Li Observed 6 Li Asplund et al., ApJ 644 (2006) Cosmological? -2.0 BBN prediction 6 Li BBN [Fe/H]

5 Big-Bang Nucleosynthesis (BBN) Theory stands on precise particle and nuclear physics! Relevant nuclear reaction rates are known within the accuracy of 5-15%! Nuclear physics is not responsible for the Li problems of factor of ~ 3 for 7 Li, 3 order of magnitude for 6 Li! R. Boyd, C. Brune, G. Fuller, and M. Smith, Phys. Rev. D82, (2010). Ref. also to: Coc, Goriely, Xu, Saimpert, and Vangioni, ApJ 744, 158 (2012) Completely unstable Some stable states Cyburt, et al., JCAP 10, 032 (2010)

6 Axion, as a Dark Matter Candidate QCD Strong CP Problem Although QCD Lagangian (i.e. strong interaction) breaks CP symmetry, CP symmetry is NOT strongly violated experimentally with neutron dipole moment. Peccei-Quinn (1977) : U(1) is dynamically broken to restore CP symmetry. Cosmological Application Erken, Sikivie, Tam & Yang, PRL 108 (2012), r g r n Axions Bose-Einstein condensates CBR-g CBR-g, reddening T g,i = 3.02 T g,f = t n t e+e- t BBN t REC t NOW time a (Axion) Nambu-Goldstone Boson n-decoupling BBN Last-Photon (3min) Scattering Bose Einstein e +- -annihilation (3.8x10 5 yr) condensates! & g-reheating

7 Hybrid Axion X 0 -DM Model h BBN h WMAP Erken, Sikivie, Tam & Yang, PRL 108 (2012), DM particle axion : Bose-Einstein condensates and cool CBRphotons after the BBN epoch (~3min) and before the re-combination (i.s. photon lastscattering) epoch (~3.8x10 5 yr). h = n B /n g, n g T g 3 h BBN < h WMAP D, overproduced! Kusakabe, Balantekin, Kajino & Pehlivan, PL B718 (2013), SUSY DM particle stau X 0 : decays to non-thermal photons g NT. Spite plateau 7 Li-overproduction, resolved! Deuteron is destroyed by D(g NT,n)p!

8 BBN Constraint on Magnetic Moment of Massive Neutrinos M. Kusakabe, A. B. Balantekin, T. Kajino & Y. Pehlivan, PR D87 (2013), Cosmological: n n + g non-therm sterile (m n =0, m n =0) sterile/active shorter t X Current Constraints Laboratory: Astrophysical: Magnetic Moment of massive neutrino X m B < m n < m B shorter t X Decoupling Temp. is Max[1MeV, m X /20]

9 CMB T-Anisotropies & Polarization including Magnetic Field Neutrino Mass Constraint Planck_reveals_an_almost_perfect_Universe Lewis 2004; Mack 2002; Challinor 2004; Kahniashvili & B. Ratra 2005; Kosowsky et al. 2005; Yamazaki et al ; Kojima et al MCMC fit to CMB anisotropies D. Yamazaki, K. Ichiki, T. Kajino, G. J. Mathews, Phys. Rep. 517 (2012), 141; PR D81 (2010), ; PR D81 (2010), TT mode

10 Likelihoodness and Probability W b h 2 W c h 2 B l (ng) n B Probability CMB Temperature and Polarization Anisotropies including Primordial Magnetic Fields and Neutrino Mass S m ν < 0.2 ev t n s log(a s ) D. Yamazaki, T. Kajino, G. J. Mathews, & K. Ichiki, Phys. Rep. 517 (2012), 141. A t /A s Probability

11 Neutrinos in Cosmology and CMB Polarization 0nbb in COUORE, NEMO3, EXO, KamLAND Zen ( < 0.1eV in the future) U 2 ebm b < 0.3 ev: COUORE, NEMO3, EXO, KamLAND Zen (2012) CMB Anisotropies + LSS ( 0.05eV in the future) m n < 0.28 ev (95% C.L.): WMAP-7yr +SPT (Benson et al. arxiv: ) < 0.36 ev (95%C.L.): WMAP-7yr + HST + CMASS (Putter et al. arxiv: ) m n < 0.2 ev (2s, B l <2nG): Yamazaki, Kajino, Mathews & Ichiki, Phys. Rep. 517 (2012), 141; PR D81 (2010), ; D77, (2009) Roles of Neutrino Anisotropic Stress CMB is affected by: -integrated Sachs-Wolfe & n free-streaming effects CMB is generated even by: -compensation mode of n-anisotropic stress (p n ) -primordial source of extra anisotropic stress (p ext ) e.g. dark radiation in brane cosmo., PMF, etc. Standard cosmology needs tuning initial condition of the inflationdriven (pre-big-bang) perturbation! Manifestation of neutrino compensation modes in polarization! 11

12 CMB from Neutrino & Extra Anisotropic Stress K. Kojima, T. Kajino & G. J. Mathews, JCAP 02 (2010), Extra anisotropic stress model Spectral index is set equal to be the WMAP-best fit value. π ext ~ r τ =10 18 Extra Primordial Anisotropic Stress Model is NOT an alternative model to INFLATION! Standard model l However, the mechanism of n (π n ) compensation makes a potential impact on π ext and n mass! π ext - Curvature perturbation is generated by Extra Anisotropic Stress π ext without assuming inflation-driven (pre-big-bang) perturbation. - It would make a great progress if we could know the nature of π ext and 12 its generation epoch before n-decoupling.

13 Yamazaki, Ichiki & Kajino, ApJ 825 (2006), L1 Yamazaki, Ichiki, Kajino, Mathews PRD, 77, (2008) (for m n = 0) Primordial Magnetic Field (PMF) could affect smaller angular scales! Upper limit: B = 7.7nG Gravitaional Wave r(t/s) < 0.43 B=5nG n B =-2.9 Lensing PMF vector mode (anisotropic stress) k 3 P(k) B 4 k 2n+6 n = n B = -3 Scale invariant. 13

14 Polarization-EE Mode for massive n Compensation to Extra-Anisotropic Stress m n = 1eV Kojima, Ichiki, Yamazaki,k Kajino & Mathews, Phys. Rev. D78 (2008), Yamazaki, Kajino, Mathews & Ichiki, Phys. Rep. 517 (2012), 141. Compensated tensor EE mode Compensated vector Passive tensor (B=3nG, n B =-2.9) 14

15 Neutrino Mass Constraints S m ν < 0.2 ev Yamazaki, Ichiki, Kajino, and Mathews, PR D81 (2010), : D. Yamazaki, T. Kajino, G. J. Mathews, and K. Ichiki, Phys. Rep. 517 (2012) 141.

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

17 Various Neutrino-Sources in Nature/Culture 1.9K CMB Cosmic Background Neutrino Cosmology verification of particle model n e, n m, n t n e Atmospheric n Direct signal of SN nneutrinos e, n m n e n e n e, n m, n t n e, n m, n t n e, n m Kamiokande (1987) n e, n m, n t Courtesy from K. Inoue Event of the Century! SN n-spectra are still unknown! T(n e ), T(n e ), T(n x )

18 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-process r-nuclei 7 Li, 11 B np-nuclei 232 Th (14.05Gy) 238 U (4.47 Gy) p-nuclei 92 Nb 98 Tc 138 La 180 Ta Cosmic Ray Spallation Li-Be-B, F, Na, etc. Mass Number A

19 Sneden, Cowan, Gallino, ARAA 46 (2008) 241. HST-obs., Roederer et al., ApJ 747 (2012) L8. log Fe/H Fe/H t y Te = Solar system -3.0 Sr-Y-Zr Ba Eu Au Pb Th U Metal-poor stars UNIVERSALITY!

20 Proton Number Z Supernova Nucleosynthesis Simulation T. Kajino & S. Chiba n-pair Heated Collapsar Model K. Nakamura, et al. IJMP (2013). 235 U 208 Pb Fe Neutron Number N

21 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

22 Tantalum( 180,181 Ta) 181 Ta g (stable), 180 Ta g (unstable, t 1/2 = 8h), 180 Ta m (isomer, t 1/2 > y) Origin of 180 Ta was unknown since SN n-process overproduces 180 Ta? The rarest isotope on the Earth & Universe! solved by Element Genesis T ne = T ne = 4 MeV! We solved dynamical explosive SN-nucleosynthesis coupled with quantum transitions simultaneously. (Hayakawa, p process et al. 2010, PR C81, ; Burbidge 2 -Fowler-Hoyle, Rev. Mod. Phys. PR C82, ) 29 (1957), Neutral current SN n-process (n e ) r process J. Burbidge M. Burbidge W. Fowler F. Hoyle

23 Galactic Chemical Evolution of 9 Be & 10,11 B Livermore Model Tn m,t = 8 MeV Woosley -Weaver 1995, ApJS 101, 181. s E n 2 Tn m,t = 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.

24 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

25 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 m, = Tn t = 6 MeV Neutrino Oscillation! n e T(n e ) < T(n e ) < T(n x ) n e MeV n m,t,n m,t e n (MeV)

26 超新星内部でのニュートリノ輸送と MSW 効果による共鳴振動 n e ( 電子型ニュートリノ ) のエネルギースペクトル Low-E comp. disappears! High-E comp. appears! t m, t t t e Center E n n e ( 電子型反ニュートリノ ) のエネルギースペクトル outside Parameters: 25M solar progenitor SN model (Hashimoto & Nomoto 1999) - sin = m 13 2 = 2.4x10-3 ev 2 - L n = 3x10 53 erg, t n = 3 sec - T ne =3.2MeV, T ne =4.0MeV, T nmt =6.0MeV E n

27 7 Li and 11 B are produced in the He/C Shell [ ] MSW high-density resonance is located at the bottom of He/C shell. n x n e n x n e

28 7 Li and 11 B are produced in the He/C Shell Suzuki, Chiba, Yoshida, Kajino and Otsuka, PRC74 (2006), Yoshida, Suzuki, Chiba, Kajino, Yokomakura, Kimura, Takamura and Hartmann, ApJ 686 (2008), 448. Suzuki and Kajino, J. Phys. G40 (2013), n x n e n x n e

29 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. - m-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

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

31 1 0.9 MSW Effect & n Mass Hierarchy Normal Mass Hierarchy Mathews, Kajino, Aoki & Fujiya, Phys. Rev. D85, (2012). 7 Li/ 11 B-Ratio Inverted Mass Hierarchy Inverted Mass Hierarchy is statistically more preferred! 74% ー Inverted 24% ー Normal Long BaselineExp. in 2011: T2K (Kamioka) MINOS Reactor Exp. in2012: sin 2 2 Double CHOOZ 13 = 0.1 First Daya Detection Bay of 7 Li/ RENO 11 B in SN-grains (KOREA) W. Fujiya, P. Hoppe, & U. Ott, ApJ 730, L7 (2011)

32 Massive Stars at birth are missing when they culminate their evolution as Supernova Explosions at death! Factor of < 2 DISCREPANCY! Expected Reasons: Half was evolved into too dark SNe to detect! 1. Failed SNe (<25M BH formation) 2. ONeMg-SNe (8-10 M ) or the mass function changed!

33 Relic Supernova Neutrinos(RSNs) for Hyper-Kamiokande (Mega-ton): Water Cherenkov J. Suzuki, T. Kajino, G. J. Mathews & J. Hidaka, ApJ (2013), submitted. No n-oscillation Atmospheric-n (final)

34 ONeMg SN Hudepohl, et al., PRL 104 (2010), fsn (failed SN) Sumiyoshi, et al., ApJ 688 (2008), 1176, + EOS (Shen et al. 1998; Lattimer & Swesty 1991). CC-SN Yoshida, et al., ApJ 686 (2008), 448; Suzuki & Kajino, J. Phys. G40 (2013) 83101; +++ J. Suzuki, T. Kajino, G. J. Mathews & J. Hidaka, ApJ (2013), submitted.

35 Expected RSN Event Rate for Hyper-Kamiokande (Mega-ton): Water Cherenkov J. Suzuki, T. Kajino, G. J. Mathews & J. Hidaka, ApJ (2013), submitted. Standard-SNe (ONeMg+CC+fSN+GRB) + MISSING-SNe Non-Adiabatic Matter (MSW) Oscillation Adiabatic Matter (MSW) Oscillation failed SNe (LS-EOS) ONeMg SNe failed SNe (Shen-EOS) failed SNe (LS-EOS) ONeMg SNe failed SNe (Shen-EOS)

36 CONCLUSION [1] Big-Bang nucleosynthesis of hybrid axion-dm model (including radiative decay of relic SUSY particles) could solve the dark matter problem and the BBN lithium problems. [2] Total neutrino mass is constrained to be S m ν < 0.2 ev from the cosmological constraints on CMB anisotropies and polarizations in the existence of the primordial magnetic field < 3nG as a source of extra-anisotropic stress. [3] Supernova n-process could determine the mass hierarchy and sin 2 13 ~ 0.1 simultaneously. Inverted hierarchy is more preferred statistically. [4] Future observation of relic supernova neutrinos (RSNs) in megaton HK water-cherenkov detector could identify the missing SN component, and also neutrino oscillation pattern, adiabatic or nonadiabatic, depending on EOS.

37 COSmology and Nuclear AstroPhysics COSNAP NAOJ & UT Nobu, thank you for your collaboration and continuous encouragement to the crossover scientists!