Cosmic Positron Signature from Dark Matter Annihilation and Big-Bang Nucleosynthesis

Transcription

1 Cosmic Positron Signature from Dark Matter Annihilation and Big-Bang Nucleosynthesis Institute for Cosmic Ray Research, University of Tokyo Kazunori Nakayama J.Hisano, M.Kawasaki, K.Kohri and KN, arxiv: J.Hisano, M.Kawasaki, K.Kohri and KN, arxiv: Institute for Cosmic Ray Research Theory Meeting (2008/12/08)

2 PAMELA found the signal of dark matter? Steep rise in the positron flux around 10~100GeV )) - )+!(e + ) / (!(e Positron excess +!(e 0.1 Contribution from DM annihilation? Positron fraction 0.02 PAMELA Expected Background Energy (GeV) Adriani et al.,arxiv:

3 ATIC found the signal of dark matter? Steep rise in the total electron and positron flux around 600GeV Contribution from DM annihilation? E e 3.0 dn/dee (m 2 s 1 sr 1 GeV 2 ) 1, ATIC BETS, PPB-BETS HEAT AMS ,000 Energy (GeV) J.Chang et al. Nature (2008) Many papers appeared after PAMELA/ATIC.

4 (Too) many papers... L.Bergstrom, T.Bringmann and J.Edsjo, arxiv: [astro-ph]; M.Cirelli and A.Strumia, arxiv: [astro-ph]; V.Barger, W.Keung, D.Marfatia, and G.Shaughnessey, arxiv; [hep-ph]; C.Chen, F.Takahashi and T.Yanagida, arxiv: [hep-ph]; I.Cholis, L.Goodenough, D.Hooper, M.Simet and N.Weiner, arxiv: [hep-ph]; M.Cirelli, M.Kadastik, M.Raidal and A.Strumia, arxiv: [hep-ph]; J.Hisano, M.Kawasaki, K.Kohri, K.Nakayama, arxiv: [hep-ph]; F.~Donato, D.~Maurin, P.~Brun, T.~Delahaye and P.~Salati, arxiv: [astro-ph]; I.~Cholis, D.~P.~Finkbeiner, L.~Goodenough and N.~Weiner, arxiv: [astro-ph]; Y.Nomura, J.Thaler, arxiv: [hep-ph], R.~Harnik and G.~D.~Kribs, arxiv: [hep-ph]; P.~f.~Yin, Q.~Yuan, J.~Liu, J.~Zhang, X.~j.~Bi and S.~h.~Zhu, arxiv: [hep-ph]; K.~Ishiwata, S.~Matsumoto and T.~Moroi, arxiv: [hep-ph]; Y.Bai and Z.Han, arxiv: [hep-ph]; P.~J.~Fox and E.~Poppitz, arxiv: [hep-ph]; C.~R.~Chen, F.~Takahashi and T.~T.~Yanagida, arxiv: [hepph]; A.~Ibarra and D.~Tran, arxiv: [hep-ph];c.~r.~chen, F.~Takahashi and T.~T.~Yanagida, arxiv: [astro-ph]; J.~Hall and D.~Hooper, arxiv: [astroph]; I.~Cholis, G.~Dobler, D.~P.~Finkbeiner, L.~Goodenough and N.~Weiner, arxiv: [astro-ph]; G.~Bertone, M.~Cirelli, A.~Strumia and M.~Taoso, arxiv: [astro-ph]; E.~Nardi, F.~Sannino and A.~Strumia, arxiv: [hep-ph]; K.Ishiwata, S.Matsumoto,T.Moroi, arxiv: [astro-ph]; J.Hisano, M.Kawasaki, K.Kohri, K.Nakayama, [hep-ph]; M.Lattanzi and J.Silk, arxiv: [astro-ph]; M.Pospelov and M.Trott, arxiv: [hep-ph]; J.Zhang, X.Bi, J.Liu, S.Liu, P.Yin, Q.Yuan, S.Zhu, arxiv: [astroph]; J.March-Russell and S.West, arxiv: [astro-ph]; J.Liu, P.Yin, S.Zhu, arxiv: [astro-ph].

5 (Too) many papers... L.Bergstrom, T.Bringmann and J.Edsjo, arxiv: [astro-ph]; M.Cirelli and A.Strumia, arxiv: [astro-ph]; V.Barger, W.Keung, D.Marfatia, and G.Shaughnessey, arxiv; [hep-ph]; C.Chen, F.Takahashi and T.Yanagida, arxiv: [hep-ph]; I.Cholis, L.Goodenough, D.Hooper, M.Simet and N.Weiner, arxiv: [hep-ph]; M.Cirelli, M.Kadastik, M.Raidal and A.Strumia, arxiv: [hep-ph]; J.Hisano, M.Kawasaki, K.Kohri, K.Nakayama, arxiv: [hep-ph]; F.~Donato, D.~Maurin, P.~Brun, T.~Delahaye and P.~Salati, arxiv: [astro-ph]; I.~Cholis, D.~P.~Finkbeiner, L.~Goodenough and N.~Weiner, arxiv: [astro-ph]; Y.Nomura, J.Thaler, arxiv: [hep-ph], R.~Harnik and G.~D.~Kribs, arxiv: [hep-ph]; P.~f.~Yin, Q.~Yuan, J.~Liu, J.~Zhang, X.~j.~Bi and S.~h.~Zhu, arxiv: [hep-ph]; K.~Ishiwata, S.~Matsumoto and T.~Moroi, arxiv: [hep-ph]; Y.Bai and Z.Han, arxiv: [hep-ph]; P.~J.~Fox and E.~Poppitz, arxiv: [hep-ph]; C.~R.~Chen, F.~Takahashi and T.~T.~Yanagida, arxiv: [hepph]; A.~Ibarra and D.~Tran, arxiv: [hep-ph];c.~r.~chen, F.~Takahashi and T.~T.~Yanagida, arxiv: [astro-ph]; J.~Hall and D.~Hooper, arxiv: [astroph]; I.~Cholis, G.~Dobler, D.~P.~Finkbeiner, L.~Goodenough and N.~Weiner, arxiv: [astro-ph]; G.~Bertone, M.~Cirelli, A.~Strumia and M.~Taoso, arxiv: [astro-ph]; E.~Nardi, F.~Sannino and A.~Strumia, arxiv: [hep-ph]; K.Ishiwata, S.Matsumoto,T.Moroi, arxiv: [astro-ph]; J.Hisano, M.Kawasaki, K.Kohri, K.Nakayama, [hep-ph]; M.Lattanzi and J.Silk, arxiv: [astro-ph]; M.Pospelov and M.Trott, arxiv: [hep-ph]; J.Zhang, X.Bi, J.Liu, S.Liu, P.Yin, Q.Yuan, S.Zhu, arxiv: [astroph]; J.March-Russell and S.West, arxiv: [astro-ph]; J.Liu, P.Yin, S.Zhu, arxiv: [astro-ph]. including me...

6 Decay or Annihilate? Decaying DM DM need not be completely stable. DM lifetime with can explain PAMELA. τ sec Flux n DM τ cm 3 s 1 Talk by Moroi-san and Takahashi-san Annihilating DM Flux n 2 DM σv cm 3 s 1 DM has weak scale annihilation cross section. σv cm 3 s 1 Cross section with can explain PAMELA.

7 Decay or Annihilate? Decaying DM DM need not be completely stable. DM lifetime with can explain PAMELA. τ sec Flux n DM τ cm 3 s 1 Talk by Moroi-san and Takahashi-san Annihilating DM Flux n 2 DM σv cm 3 s 1 DM has weak scale annihilation cross section. σv cm 3 s 1 Cross section with can explain PAMELA.

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9 Dark matter annihilation in the Galaxy now Positron, Gamma-ray, Neutrinos,...

10 Dark matter annihilation in the early Universe Effects on Big-Bang Nucleosynthesis Dark matter annihilation in the Galaxy now Positron, Gamma-ray, Neutrinos,...

11 Contents Positron Flux Effects on Big-Bang Nucleosynthesis Gamma-Ray Flux Anti-proton Flux Neutrino Flux

12 Positron Flux

13 Positron from DM Annihilation Kamionkowski,Turner(91), Baltz,Edjso(98),... χχ W + W, b b, l + l,... e ±, γ, p, ν,... Energy loss due to synchrotron radiation and inverse Compton with CMB and star light. High-Energy positron can reach to the Earth within a few kpc. L Positron flux is not so sensitive to diffusion zone L and halo density profile.

14 Propagation of positrons in Galaxy Diffusion Equation Φ t = K(E) 2 Φ(E) + Diffusion E [b(e)φ(e)] + Q(E) Energy loss by synchrotron and inverse compton Source term from DM annihilation e + r K(E) cm 2 s 1 (E/1GeV) 0.6 b(e) GeVs 1 (E/1GeV) 2 Typical propagation distance w/o energy loss r 1 kpc(100gev/e) 0.2

15 Positron-to-electron ratio : Main Annihilation mode : e + e σv cm 3 s 1 µ + µ σv cm 3 s 1 W + W σv cm 3 s 1 R(E) R = Φ e + Φ e + Φ e +

16 Positron-to-electron ratio : Main Annihilation mode : e + e σv cm 3 s 1 µ + µ R(E) R = Φ e + Φ e + Φ e + σv cm 3 s 1 W + W σv cm 3 s 1 Wino (Super partner of W boson) is a good candidate

17 L=1kpc J.Hisano, M.Kawasaki, K.Kohri, KN (2008)

18 Wino with mass around 200GeV fits the PAMELA data L=1kpc J.Hisano, M.Kawasaki, K.Kohri, KN (2008)

19 Effects on BBN

20 Effects of DM Annihilation on BBN Lithium Problem Observation of metal-poor stars Jedamzik (2004) Hisano,Kawasaki,Kohri,KN(2008) log 10 ( 7 Li/H) obs = 9.90 ± 0.09 Bonifacio et al. (2006) ( 6 Li/ 7 Li) obs = ± Aspuland et al. (2006) Standard BBN cannot explain these values. Hadron injection in BBN era from DM annihilation can help the situation. Otherwise, BBN gives constraint on DM models.

21 χχ W + W, b b, l + l,... hadrons, radiation Destruction/production of light elements 7Li destruction 7 Be(n, p) 7 Li(p, 4 He) 4 He 4 He, 3 He, D, 6 Li, 7 Li 6Li Production p(n) + α BG T, 3 He,... T( 3 He) + α BG n(p) + 6 Li 6Li production and many other processes...

22 Assuming W-boson injection J.Hisano, M.Kawasaki, K.Kohri, KN (2008)

23 200GeV Wino also solves lithium problem! Assuming W-boson injection J.Hisano, M.Kawasaki, K.Kohri, KN (2008)

24 Gamma-Ray Flux

25 Gamma-ray from DM Annihilation Bergstrom, Ullio, Buckley(98), χχ W W, bb, l l,... ± e, γ, p, ν,... Continuum gamma Flux: "σv# dnγ Φγ (ψ, E) 4πm2DM de Particle physics model Flux depends sensitively on halo profile.! ρ2 (l)dl(ψ) l.o.s. DM density profile ρ0 Isothermal ρ(r) 1 + (r/a)2 NFW ρ(r) ρ0 (r/a)(1 + (r/a))2

26 Expected Gamma-Ray flux from the Galactic Center for NFW and isothermal profile. Fermi telescope will confirm this scenario The case of Wino DM 5 < l < 5 2 < b < 2 J.Hisano, M.Kawasaki, K.Kohri, KN (2008)

27 Anti-Proton Flux

28 Anti-Protons from DM Annihilation Bergstrom, Edsjo, Ullio(99), Donato et al. (01),... χχ W + W, b b, l + l,... e ±, γ, p, ν,... (m p m e ) Energy-loss is not effective. Easily escape from the diffusion zone. Anti proton flux sensitively depends on the choice of diffusion zone. L L Degeneracy between diffusion const. and L. consistent with B/C ratio. Degeneracy does not hold for DM-originated anti-proton flux.

29 Anti-proton flux from 200GeV Wino max L = 15kpc med L = 4kpc min L = 1kpc Consistent with observational data.

30 Neutrino Flux

31 Neutrino Signal from DM Annihilation Ritz, Seckel (88),Kamionkowski (90),... χχ W + W, b b, l + l,... e ±, γ, p, ν,... High energy neutrinos from the Galactic center Interaction inside the Earth High-energy Muons ν detector µ Earth Search for up-going muons Limits from Super-K

32 ν µ µ ν µ µ Cross section for σ (µ) ν G2 F s π Muon energy loss de = a be dx µ s = 2m N E ν W N N Ionization loss : a 2 MeVcm 2 g 1 Pair production, brems,... : b 10 6 cm 2 g 1 Muon Flux at SK production F µ Muon range: Primary Neutrino Flux R µ E de df ν de E2 de

33 Limits from SK : DM annihilation which can explain ATIC must not produce neutrinos with same rate. m = 800GeV σv ann = cm 3 s 1 ν s l ± s from the GC J.Hisano, M.Kawasaki, K.Kohri, KN (2008)

34 ATIC favors heavy DM with large cross section. σv ann cm 3 s 1 m = 620GeV m = 800GeV

35 Summary Dark matter annihilation can explain observed positron/electron excess by PAMELA/ATIC. Effects on BBN Gamma-ray Flux Anti-Proton Flux Neutrino Flux Constraints on DM model, or may be another hint for DM annihilation. And of course, the LHC may discover the DM. We are now in the vicinity of DM detection!

36 Back-up Slides

37 Notes Standard thermal relic DM Ω DM 0.1 ( cm 3 s 1 σv ) PAMELA/ATIC σv cm 3 s 1 We must give up standard thermal relic scenario or introduce large boost factor (BF~100) In the case of wino, gravitino decay can produce correct amount of wino if T R GeV

38 Anomaly-mediation Randall, Sundrum (98) Giudice,Luty,Murayama,Rattazzi (98) SUSY breaking effect is transmitted via super-weyl anomaly effect. m B = 11g 2 16π 2 m 3/2 m W = g2 16π 2 m 3/2 m g = 3g2 s 16π 2 m 3/2 LSP Tachyonic slepton Universal scalar mass (MAMSB) LSP is wino like Large annihilation cross section HIsano,Matsumoto,Nagai,Saito,Senami(05) Hidden brane MSSM brane SUSY!"!"!#%!#$ :4)';:**)*/'95:4)549:)<< &'())*)))+ %!!!#2!(),)"-!)./0!" "-#!!" ()&)1/0)+

39 Neutrinos from the Sun Neutralinos accumulated in the Sun annihilate High energy neutrinos Evolution of neutralino number in the Sun Ṅ = C A N 2 N : number of neutralinos trapped in Sun A : annihilation rate C : trapping rate Ritz, Seckel(88), Kamionkowski(91),... σv /V ( ) sec 1 σ (SD) H cm 2. Static solution Γ = 1 2 A N 2 = 1 2 C Neutrino flux depends on scattering cross section with H

40 Minimal anomaly-mediation model (MAMSB) m 3/2 tan β Constraint: b sγ m h > 114GeV m 0 :Gravitino mass :Universal scalar mass :Ratio of up- and down-type Higgs VEV M.Nagai, KN(08) Current bound (SK) Muon signal is enhanced only when the gaugino-higgsino mixing is large. IceCube sensitivity : Φ µ 80 km 2 yr 1

41 Direct Detection CDMS, XENON10... XENON100, XMASS, Super-CDMS,... Neutralino-nucleon scattering Kinetic energy is transferred to nucleon. E m DM v 2 100keV Ionization, Scintillation, Heating signal XENON10 From XENON homepage

42 Dominant process : Higgs exchange Gaugino-higgsino mixing χ N h χ N M.Nagai, KN(08) is important Current bound (CDMS) Direct detection rate is enhanced only when the gaugino-higgsino mixing is large. SuperCDMS : σ SI cm 2