Mathews Grant J. (University of Notre Dame) Boyd Richard N. (Lawrence Livermore National Laboratory) 2009/5/21

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1 Mathews Grant J. (University of Notre Dame) Boyd Richard N. (Lawrence Livermore National Laboratory) 2009/5/21

2 Abstract strongly interacting massive particles (SIMPs, X) Big Bang (BBN) X heavy colored particle

3 1. Introduction BBN Li BBN SIMP relic abundance

4 Introduction [1(2,3)4 ] C 3+4+Q s-wave 1+2 Q 3+4

5 ) detailed balance 4 (1,2,3,4) Q-value γ 15 N(p,α) 12 C σ(2mev)=0.5 b 3 He(α,γ) 7 Be σ(2mev)=10-6 b p(p,e + ν e )d σ(2mev)=10-20 b 1b=10-24 cm 2

6 Big Bang Big Bang 200 MeV QCD MeV Big Bang 0.3eV ħ 0.2meV [ ] Gauge? Neutrino Background Any signature of new physics? 3K Background

7 H,He (BBN) C Ca ( ) NSE (Ia ) Ryan 2000 Li,Be,B ( + ) [ ] D, 3 He, 4 He: BBN 6 Li: (CRN) 7 Li: BBN+CRN+ ν 9 Be, 10 B: CRN 11 B: CRN+ ν D : QSO 3 He : HII 4 He : metal-poor outer galaxies HII 6,7 Li : Metal-Poor Halo Stars

8 Big Bang (SBBN) n p (n/p) EQ =exp(-q/t) Q m n -m p =1.293MeV t~1sec,t=t F ~1MeV( freeze-out) photon decouple (νν e + e - γγ) n p freeze-out (n/p) freeze-out =exp(-q/t F )~1/6 Kawano code (1992) (1MeV= K) Rates Smith et al. (1993) +Descouvemont et al. (2004) +Cyburt & Davids (arxiv: ) 7 Li(p,α) 4 He τ n =881.9s (Mathews et al. 2005, average) T(α,γ) 7 Li 3 He(α,γ) 7 Be D(α,γ) 6 Li 6 Li(p,α) 3 He T 9 T/(10 9 K) e - 7 Be 7 Li η=n b /n γ = WMAP

9 SBBN SBBN: baryon-to-photon ratio η η=(6.27±0.17) (WMAP: Dunkley et al. 2008) Metal-Poor Halo Star (MPHS) 7 Li CMB+SBBN factor~3-4 6 Li Li

10 6,7 Li

11 [ 6 Li ] α α α+α (Montmerle 1977) (Rollinde et al. 2005) (Suzuki & Inoue 2002) log( 6,7 Li/H)+12 Stellar depletion? 7 Li Asplund et al. (2006) 7 Li BBN ejectaα+ α α+α (Nakamura et al. 2006) MPHS 3 He 4 He( 3 He,p) (Tatischeff &Thibaud 2007) Inoue et al. (2005) 6 Li? 10 3 [ 6,7 Li ] ( ejection) MPHS -2.0 (Richard et al. 2005) 6 Li BBN [Fe/H]=log{(Fe/H)/(Fe/H) } (Piau et al. 2006)

12 exotic (Ellis et al , Reno & Seckel 1988, Dimopoulos et al , Kawasaki et al , ) exotic exotic (Pospelov 2007, Kohri & Takayama 2007, Kawasaki et al , Hamaguchi et al. 2007, ) The WMAP Science Team (e.g. slepton(nlsp) (Feng et al. 2003) gluino(split SUSY) (Arkani-Hamed et al. 2005) SBBN 6,7 Li

13 Li, Be, B 1 (n p) (Wikipedia) 11 B 10 B 9 Be

14 m p m d1 +m d2 m A +m X m AX shock

15 X - BBN X - A A X X (Cahn & Glashow 1981) X - X - (e.g. Kohri & Takayama 2007, Bird et al. 2008) A X - X - A γ X X (e.g. Kohri & Takayama 2007) a X - A X - B b X - (Jittoh et al. 2007, Bird et al. 2008) X - A Y 0 B X - (Pospolov 2007, Cyburt et al. 2006) a X - A X - A+a

16 X (Bird et al. 2008) p X (Kusakabe et al. 2007, Pospelov 2007) p X - 7 Be X - 7 Be X - γ 8 B X - 8 B X - 8 γ B * X - 8 B 8 B 1 + X 7 Be X (p,γ) 8 B X Phys. Rev. D76 (2007) 7 Be+p 8 B*(1 + ) 8 B+γ E th ~30keV 7 Be X 7 Li E th 7 Be X +p 8 B*(1 + ) X 8 B X 2 +

17 Abundance network 7 Be X 7 Li+X 0 Nuclear flow (case 1) m x >>1GeV, n x =0.05n b, τ x = η= He X (d,x - ) 6 Li (Pospelov 2007) 7 Be X +p 8 B X *a 8 B X +γ (Bird et al. 2008) 7 Be(X -,γ) 7 Be X X - X 9 Kusakabe et al.(2007) T 9 =T/(10 9 K)

18 network Li : d( A Li)= A Li Calc / A Li Obs d( 6 Li)=10 η= Li Li overproduction d( 6 Li) d( 7 Li) 7 Li 3 Y X =n X /n b 7 Li 6 Li : Y X and τ X (1-3)x10 3 s

19 X 0 BBN

20 Colored Particles Y relic abundance Kang et al. (2008) Y - Y Y n Y /s~10-14 (n Y /n b ~10-4 ) X π T<T c ~180MeV X BBN

21 X 0 BBN X 0 BBN (Dicus & Teplitz 1980) N-X N-Λ BBN X 4 He 4 He X 2 H, 3 H, 3 He X 4 He X / 4 He BBN X Be 8 Be X / 9 Be 4 He X X (Mohapatra & Teplitz 1998) X X

22 1. X 0 [ ] X spin 0, charge 0, mass m X >>1 GeV X 1)N-X n-p X 2) Woods-Saxon (V 0 =50MeV, a=0.6fm, R=<r m2 > 1/2 ) r X 0 A Schrödinger ~Ο(10MeV) X!

23 2. X Q-value i) X : A(X,γ)A X A(n,γ)B p(x,γ)p X, p X (p,γ)pp X, p X (n,γ)d X RADCAP (Bertulani 2003) ii) : A X (n,γ)b X E1 hindered A(n,γ)B 10-3 iii) : X Q-value

24 iv) A X (n,p)b X A(n,p)B 2. X v) X : p X (n,p)n X 7 Be(n,p) 7 Li n p n p X:massive & strong interaction vi) X : p X (α,p) 4 He X 8 B(α,p) 11 C vii) β : SBBN β Q-value Q-value

25 O X 3. network 14 O X 15 O X 16 O X 12 N X 13 N X 14 N X 15 N X 10 C X 11 C X 12 C X 13 C X 14 C X 8 B X 9 B X 10 B X 11 B X 12 B X 6 Be X 7 Be X 8 Be X 9 Be X 10 Be X 5 Li X 6 Li X 7 Li X 8 Li X pp X 3 He X 4 He X 5 He X 6 He X 1 H X 2 H X 3 H X 1 n X X β X : 25 X : 147 β : 15 X : 2 X-decay: 38

26 Abundance X-capture Nuclear flow m x >>1GeV, n x =10-8 n b, τ x = T 9 ~5: X T 9 1: 2 H X 3 He X T 9 ~1: d (d,p), (d,n) X 13 C X Dicus & Teplitz (1980), Mohapatra & Teplitz (1998)! T 9 =T/(10 9 K)

27 Abundance Nuclear flow m x >>1GeV, n x =10-8 n b, τ x = T 9 ~5: X T 9 1: 2 H X 3 He X T 9 ~1: d (d,p), (d,n) X 13 C X X-capture X 0 X - 5 Li X 5 He X X 0 T 9 =T/(10 9 K)

28 X 0 Abundance Y X =n X /n b η= Be, B BBN 10 B/ 11 B~10 5 B ( 10 B/ 11 B~0.4) ν-process( 10 B/ 11 B<<1) relic abundance Y X 10-8 τ X τ X 6 Li, 7 Li X 0 7 Li, B, 9 Be

29 X 0 BBN X 0 X 0 X Q X 0 X BBN [ ] BBN T 9 ~5 X 0 T 9 ~1 D D X X X 6 Li, 7 Li X 0 relic abundance n X /n b ~10-8 τ X

Big Bang Planck Big Bang 1 43 Planck Planck quantum gravity Planck Grand Unified Theories: GUTs X X W X 1 15 ev 197 Glashow Georgi 1 14 GeV 1 2

Big Bang Planck Big Bang 1 43 Planck Planck quantum gravity Planck Grand Unified Theories: GUTs X X W X 1 15 ev 197 Glashow Georgi 1 14 GeV 1 2 12 Big Bang 12.1 Big Bang Big Bang 12.1 1-5 1 32 K 1 19 GeV 1-4 time after the Big Bang [ s ] 1-3 1-2 1-1 1 1 1 1 2 inflationary epoch gravity strong electromagnetic weak 1 27 K 1 14 GeV 1 15 K 1 2 GeV

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