Nucleosynthesis in Supernovae and the Big-Bang II

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1 IV International Summer School 2005 Center for Nuclear Study, University of Tokyo August 18 23, 2005 Nucleosynthesis in Supernovae and the Big-Bang II Taka Kajino National Astronomical Observatory Department of Astronomy, University of Tokyo

2 Solar System Abundance BIG-BANG Constrains Ω B and Cosmological Thoeries of Ω CDM & Ω Λ! STARS R-PROCESS R-process ELEMENTS elements, UNKNOWN SUPERNOVAE SITES?? R S N=50) 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?

3 OUTLINE Universe is likely flat and accelerating! Ω B + Ω CDM + Ω Λ = 1 Six (eleven) Parameters! Is BARYON, Ω B = 0.04, consistent with Big-Bang Cosmology and Nucleosynthesis (as a CANDLE of dark side of the Universe)? BBN constrains Brane Cosmology! What is the nature of CDM, Ω CDM = 0.26? Disappearing CDM Model in Brane World Cosmology! Ichiki, Garnavich, Kajino, Mathews & Yahiro, PRD 68 (2003) What is DARK ENERGY, Ω Λ = 0.7? Growing CDM Model in Brane World Cosmology! Umezu, Ichiki, Kajino, Mathews Nakamura & Yahiro,(2005) (astro-ph/ ) COSMIC AGE ( Gy), strongly model-dependent? Supernova R-Process & Origin of 232 Th, 235,238 U! --- Model independent! Sasaqui, Kajino & Balantekin, ApJ (2005), in press. (astro-ph/ )

4 The Universe is homogeneous and isotropic in a large enough scale. T = K δt < 18 µk 2dF Quasar (Matter) Distribution: Homogeneous Cobe Sky Maps of CMB; Isotropic

5 Newtonian Equation Birkoff s Theorem: Gravity due to mass interior to an arbitrary sphere. r(t) M m E = 1 2 m r Ý 2 GmM r 1 2 m r Ý 2 = Gm[(4 / 3)πρr 3 ] r x 1/2mr 2 + E M = 4/3πρr 3 r Ý r 2 = 8 3 πgρ + 2 E mr 2

6 General Relativity G µν = R µν 1 2 Rgµν = 8π GT µν +Λg µν R µν = R λ µλν = λ Γ λ λ µν ν Γ µλ + Γ λ ηλ Γ η µν Γ λ η ην Γ µλ Γ λ µν = 1 { 2 gλβ ν g βµ + µ g βν β g } µν 1 g µν = a 2 (t) 1 kr 2 a 2 (t)r 2 a 2 (t)r 2 sin 2 θ T µ ν = ρ p p p

7 Einstein Equation Newtonian Equation Space-space component G 00 = 8π GT 00 + Λg 00 H 2 = (v/r) 2 -k = E/m Friedmann Eq. H 2 = 8 3 πgρ + k + Λ a 2 3 Cosmological Constant r Ý r 2 = 8 3 πgρ + E mr 2 H 2 2 = H 0 Ω γ a 4 + Ω M a 3 + Ω k a 2 +Ω Λ Ω α = ρ α /ρ C ρ C = 3H 02 /8πG a = a(t) = scale factor = r Deceleration parameter q 0 = (d 2 r/dt 2 )/rh 2 = [Ω CDM /2 Ω Λ ] Ω CDM /2 Ω Λ acceleration!

8 Cosmic Expansion History accelerating Ω MCM Ω Λ decelerating critical closed

9 Cosmic Microwave Background Anisotropies WMAP δt T = l C l a lm 2 m a lm Y lm (θ,φ) C l = δt/t(n) δt/t(n+θ)

10 Cosmological Parameter Dependence Larger Ω Λ Larger Ω CDM Larger Ω B Baryon Drag Multipole l Dark Matter potential Ω CDM Baryon Mass Ω B Tγ Photon Pressure

11 Pie Chart of Cosmic Mystery t = 3 x 10 5 yr Ordinary matter makes up a small fraction of mass/energy. Dark matter and dark energy dominate. Ω Λ Ω B Ω CDM

12 The Power of BBN is that the Physics is Accessible Thermodynamic Equilibrium of Particles and Nuclei Cosmic Expansion Nuclear Reactions

13 PRIMARY PROCESSES Big-Bang Nucleosynthesis Supernova R-Process Initially p& n NSE α-process R-process (neutron-rich)

14 Evolution of Abundances p n d 4 He NSE 3 He t 7 Li 7 Be 6 Li Dymanical Nucleosynthesis p 4 He d t 3 He n 7 Li 7 Be 6 Li

15 Big-Bang Nucleosynthesis (BBN) Diagram CMB (WMAP) t = 3 min Big-Bang Nucleosynthesis Constraints BBN- 4 He Cosmic Baryon Density Ω B Ω B s from BBN and CMB are inconsistent!

16 NEW MEASUREMENT OF NEUTRON LIFE Serevlov et al., Phys. Lett. B605 (2005), 72 ULTRA-COLD NEUTRON δτ n /τ n = -1 % STANDARD QUARK MODEL KMS (Kobayashi-Masukawa- Cabbibo) MATRIX N P V ud d u : V ud

17 Effect of Neutro-Life on BBN- 4 He : 2p + 2n 4 He 1st effect: δτ n δt d δ(n/p) δ( 4 He) 2nd effect: δτ n δn δ( 4 He) NET EFFECT: δτ n < 0 δ( 4 He) < 0

18 Big-Bang Nucleosynthesis vs. CMB Mathews, Kajino & Shima, PRD71 (2005) (R) 4 He CMB - WMAP CONSISTENT! 7 Li PROBLEM!?

19 7 Li Abundance in Halo Dwarf Stars Ryan, Kajino, Beers, Suzuki, Romano, Matteucci & Rosolankova 2001, ApJ 549, 55. Is this plateau really Big-Bang origin? [Fe/H] Affected by SN ν-process? SN II Nucleosynthesis contributes!

20 SN1987A SNe II Nucleosynthesis can produce 7 Li and 11 B as the BBN does in the early Universe! Supernova ν - process!

21 Before Explosion Yoshida, Kajino & Hartman, Phys. Rev. Lett. 94 (2005), After Explosion

22 Yoshida, Terasawa, Kajino & Sumiyoshi, Astrophys. J. 600 (2004), 204. Yoshida, Kajino & Hartman, Phys. Rev. Lett. 94 (2005), Calibrate ν-temperature! Constrain ν-oscillation?

23 Primordial 7 Li Abundance, observed? Ryan, Kajino, Beers, Suzuki, Romano, Matteucci & Rosolankova 2001, ApJ 549, 55. SN ν -PROCESS GCR + STARS [Fe/H] Primordial 7 Li is NOT affected by the SN ν -PROCESS! Nuclear Physics can solve 7 Li PROBLEM?

24 BBN Nuclear Uncertainties are Improving Reaction Needed d(p,γ) 3 He 3.2% d(d,n) 3 He 2.0% d(d,p) 3 H 1.6% 3 He(α,γ) 3 He 2.3% Descouvemont, Adahchour, Angulo, Coc, Vangioni-Flam. ApJ, (2004) Nollett & Burles, PRD, 61, (2000)

25 7 Be (d, p) 2α PRPROSAL of Coc et al. (2003) Astrophysical S-factor (kev b) Data from Kavanagh (1960) If cross section were EXTREMELY larger, then, 7 Be would be destroyed! Big-Bang Energy E cm (MeV)

26 Big-Bang Nucleosynthesis Coc, Vangioni-Flam, Descouvemont, Adahchour & Angulo, ApJ 600 (2004) 544. New neutron life! Mathews, Kajino and Shima, PRD71 (2005) (R) Lyman-α! 7 Be If 7 Be would be destroyed, then Ω B s from BBN and WMAP could be consistent! WMAP

27 7 Be (d, p) 2α Angulo et al. (2005) EXPERIMENT Data from Kavanagh (1960) Not very largely enhancement! Primordial 7 Li should be high!! Big-Bang Energy E cm (MeV)

28 PRIMARY PROCESSES Big-Bang Nucleosynthesis Supernova R-Process Initially p& n NSE α-process R-process (neutron-rich)

29 INHOMOGENEOUS BIG-BANG NUCLEOSYNTHESIS Kajino and Boyd, ApJ 359 (1990) 267; Orito, Kajino, Boyd & Mathews, ApJ 488 (1997) Be 7 Li(n,γ) 8 Li (n,γ) 9 Li(e - ν) 9 Be, Inhomogeneous Big-Bang 7 Li(t,n) 9 Be, 7 Li( 3 He,p) 9 Be 7 Li(n,γ) 8 Li(α,n) 11 B Standard Big-Bang 7 Li(α,γ) 11 B

30 OUTLINE Universe is likely flat and accelerating! Ω B + Ω CDM + Ω Λ = 1 Six (eleven) Parameters! Is BARYON, Ω B = 0.04, consistent with Big-Bang Cosmology and Nucleosynthesis (as a CANDLE of dark side of the Universe)? BBN constrains Brane Cosmology! What is the nature of CDM, Ω CDM = 0.26? Disappearing CDM Model in Brane World Cosmology! Ichiki, Garnavich, Kajino, Mathews & Yahiro, PRD 68 (2003) What is DARK ENERGY, Ω Λ = 0.7? Growing CDM Model in Brane World Cosmology! Umezu, Ichiki, Kajino, Mathews Nakamura & Yahiro,(2005) (astro-ph/ ) COSMIC AGE ( Gy), strongly model-dependent? Supernova R-Process & Origin of 232 Th, 235,238 U! --- Model independent! Sasaqui, Kajino & Balantekin, ApJ (2005), in press. (astro-ph/ )

31 Brane World Cosmology SUSY!? 5 th dimension, compactified.

32 Disappearing LSP (Lightest SUSY Particle) CDM Model Is a likely possibility! vs. m B ~ 1 GeV LSPs (CDM) disappear at cosmological time! BARYONS do not!

33 Modified Friedmann Equation E = Dark Radiation or Electric part of the bulk Weyle tensor Ichiki, Garnavich, Kajino, Mathews & Yahiro PRD 68 (2003),

34 Thermal History of the Universe INFLATION: (GW) QCD phase tr ν-dec, e + e - -annihi Observables at different cosmic time! BBN (Big-Bang Nucleosynthesis) Matter-Dom Era CMB Anisotropies Rad-Dom Era Type Ia SNe, CLUSTER M/L sec 3 min 10 5 y 1-10 Gy

35 t = 3 min t = 3x10 5 y BBN CMB Anisotropies Ω Λ PEAK Dark Radiation Dark Radiation / Photon - Energy Type Ia Supernovae t = 1-10 Gy CLUSTER M/L ratio t = 1-10 Gy

36 Constraints on SUSY-Brane Cosmology (Disappearing CDM) Model Ichiki, Garnavich, Kajino, Mathews & Yahiro, PRD 68 (2003) Dark Energy is still needed! Our Model is as good as the standard model.

37 Brane World Cosmology CDM particles can exist in the bulk. Then, they can FLOW IN from the bulk! 5 th dimension, compactified. Dark Enerfy term: q = adjustable parameter We propose Growing-CDM Model for DARK ENERGY! Ω Λ = 0 model!

38 Supernova z vs. m-m Relation t = 1-10 Gy Standard ΛCDM model Ω Λ = 0.71 Our best-fit model Ω Λ = 0

39 CMB Anisotropies t = 3x10 5 y Our best-fit model Ω Λ = 0 Standard ΛCDM model Ω Λ = 0.71 Only OUR MODEL can explain this quenching! Cosmic Variance?

40 Cosmic Microwave Background WMAP shows evidence for suppression of quadrupole and octopole moments. - Aligned in the direction of Virgo: Tegmark et al (2003) - This could suggest a compact cosmology - Use axis to guide search (l,b) ~ (-80,60 )

41 Matter Power Spectrum P(k) t = 1-10 Gy Standard ΛCDM model Ω Λ = 0.71 Our best-fit model Ω Λ = 0

42 Conclusion Big-Bang Nucleosynthsis is one of the Pillars of very precise Particle-Nuclear Theory and Modern Cosmology. Standard Quark Model --- KMC Matrix! Dark Matter --- SUSY Particles in Brane Cosmology Dark Energy --- Flowing in of CDM in Brane Cosmology Acceleration, due to CDM inflow without Ω Λ! Quenching of low multipoles in CMB, due to late ISW effect! Li problem still remains?? Core-Collapse Supernovae are Viable Astrophysical Sites for R-Process. New Role of R-Process Elements 232 Th & 235,238 U --- Cosmochronology for Metal-Deficient Stars, hopeful but needs more precision? --- Sensitivity of Neutrino Cutoff to BH vs. NS Formation!