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High energy n astronomy and Gamma-ray bursts

High energy n astronomy and Gamma-ray bursts. Eli Waxman Weizmann Institute, ISRAEL. Outline. The origin of UHECRs (>10 19 eV): Unknown Part I: UHECR-GRBs Part II: The role of n astronomy. What do we know about >10 19 eV CRs?. J(>10 11 GeV)~1 / 100 km 2 year 2 p sr

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High energy n astronomy and Gamma-ray bursts

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  1. High energy n astronomy andGamma-ray bursts Eli Waxman Weizmann Institute, ISRAEL

  2. Outline • The origin of UHECRs (>1019eV): Unknown • Part I: UHECR-GRBs • Part II: The role of n astronomy

  3. What do we know about >1019eV CRs? • J(>1011GeV)~1 / 100 km2 year 2p sr • Most likely X-Galactic (RL=e/eB=40ep,20kpc) • Composition? HiRes- p, Auger- becoming heavier? (Uncertain spp) • (An)isotropy: 2s, consistent with LSS • Production rate & spectrum: protons, e2(dQ/de) ~1043.7 erg/Mpc3 yr + GZK • Acceleration (expanding flow): Confinement L>LB>1012 (G2/b) (e/Z 1020eV)2 Lsun Synch. losses G > 102.5 (L52)1/10 (dt/10ms)-1/5 !! No L>1012 Lsun at d<dGZK  Transient Sources [EW 95]

  4. UHECR sources: Suspects • Constraints:- L>1012 (G2/b) Lsun • - e2(dQ/de) ~1043.7 erg/Mpc3 yr • - d(1020eV)<dGZK~100Mpc • !! No L>1012 Lsun at d<dGZK  Transient Sources • Gamma-ray Bursts (GRBs) • Lg~ 1019LSun>1012 (G2/b) Lsun= 1017 (G/ 102.5)2 Lsun • G~ 102.5 (L52)1/10 (dt/10ms)-1/5 • e2(dQ/de)g~ 1053erg*10-9.5/Mpc3 yr = 1043.5 erg/Mpc3 yr • Transient: DTg~10s << DTpg ~105 yr • Active Galactic Nuclei (AGN, Steady): • G~ 101 L>1014 LSun=few brightest • !! Non at d<dGZK  Invoke: • * “Dark” (proton only) AGN • * L~ 1014 LSun , Dt~1month flares • (from stellar disruptions) [EW 95, Vietri 95, Milgrom & Usov 95] [EW 95] [Blandford 76; Lovelace 76] [Boldt & Loewenstein 00] [Farrar & Gruzinov 08]

  5. UHECR per GRB • Uncertainties: Absolute ECR calibration ECR/EUHECR z=0 high-L GRB rate [Guetta et al. 2010]

  6. GRB int./ext. shock acceleration Confinement L>LB>1012 (G2/b) (e/Z 1020eV)2 Lsun • LB~Lg ?? • Internal shocks (G~1): B~Bequip, LB~L Does not necessarily require orders of magnitude amplification

  7. GRB int./ext. shock acceleration Shock frame G p • External (G>>1): Bup~10-5 Bequip ?? LB<<L, No UHE acceleration?? • e- t(acceleration) < t(IC) X-ray AG  B > 0.2 n05/8 mG >> 1mG 100MeV  B > 5 n05/8 mG (0.1mG )  Upstream field generation, Possible UHE @ external Consistent with theoretical considerations (Kumar & Barniol-Duran 09: No amplification? Parameter fit {eB, ee…} ignoring physics) Downstream Upstream [Li & EW 06] [Li 10] [Piran &Nakar 10] [eg Keshet et al 09; Nishikawa et al. 09]

  8. HE n Astronomy • p + g N +p p0 2g ; p+  e+ + ne + nm + nm  Identify UHECR sources Study BH accretion/acceleration physics • E2dQ/dE=1044erg/Mpc3yr & tgp<1: • If X-G p’s:  Identify primaries, determine f(z) [EW & Bahcall 99; Bahcall & EW 01] [Berezinsky & Zatsepin 69]

  9. HE n experiments Optical Cerenkov - South Pole Amanda: 660 OM, 0.05 km3 IceCube: +660/yr OM (05/06…) 4800 OM=1 km3s - Mediterranean Antares: 10 lines (Nov 07), 750 OM 0.05 km3 Nestor: (?)  0.1 km3 km3Net: R&D  1 km3 • UHE: Radio Air shower • Aura, Ariana (in Ice) Auger (nt) • ANITA (Balloon) EUSO (?) • LOFAR

  10. GRB n’s • If: Baryonic jet • Background free: [EW & Bahcall 97, 99; Rachen & Meszaros 98; Guetta et al. 01; Murase & Nagataki 06]

  11. GRB G & fpp • Prompt ~1MeV synch  fpp ~ tgg(100MeV)~1 tgg(100MeV)~1 G~300 Prompt GeV photons  tgg(100MeV)<<1, G>>300, no n’s ?? Is tgg(100MeV)<<1? • Challenge to prompt MeV sync production • 95% of LGRB not detected by LAT For bright GRBs, non detection implies: F(>100MeV)/F(1MeV) < 0.1  tgg(100MeV)>~1 ? [Abdo et al. 09; Greiner et al. 09; Dermer 10] [Guetta et al. 10]

  12. GRB G’s • Caution in inferring Gmin: - No exponential cutoff at tgg>1, rather nfn~1/n - GeV & MeV emission likely originate from different radii (HE delay), n(tgg=1)~R • Internal collisions at R0“residual” coll. @ R>> R0 E(R)~1/Rq with q<2/3 nfn~1/nq for n>n(tgg=1,R= R0) May account for: prompt optical (avoid self-abs.) prompt GeV (avoid pair prod.) GRB080916c HE delays  G~300 [Li & EW 08] [Li 10] [Li 10]

  13. The current limit [Achterberg et al. 08 (The IceCube collaboration)]

  14. TeV GRB n’s • Collapsar jet penetration, failed SN jet : TeV n’s [Meszaros & EW 01; Razzaque et al. 03, 04; Guetta & Granot 03; Dermer & Atoyan 03 Ando & Beacom 05]

  15. n- physics & astro-physics [EW& Bahcall 97] • p decay  ne:nm:nt = 1:2:0 (Osc.) ne:nm:nt = 1:1:1 t appearance experiment • GRBs: n-g timing (10s over Hubble distance) LI to 1:1016; WEP to 1:106 • EM energy loss of m’s (and p’s) • ne:nm:nt = 1:1:1 (E>E0) 1:2:2 • GRBs: E0~1015eV • Combining E<E0, E>E0 flavor measurements may constrain CPV [SinQ13 Cosd] [EW & Bahcall 97; Amelino-Camelia,et al.98; Coleman &.Glashow 99; Jacob & Piran 07] [Rachen & Meszaros 98; Kashti & EW 05] [Blum, Nir & EW 05]

  16. Summary UHECRs • Origin- an outstanding puzzle • GRBs- only known sources satisfying all constraints n astronomy • Detectors approach required ~1Gton scale • Resolve UHECR puzzle: composition, sources • Resolve GRB physics open Q: Baryonic/Poynting jet, G, particle acceleration [test collapsar jets, X/FUV flares] • Constrain n physics, LI, WEP

  17. Composition clues HiRes 2005 Auger 2009 Protons Heavier at highest E? Or: modified s extrapolation? (s~300 TeV) [E.g. Wibig 08,09; Ulrich et al. 09 Kusenko 10]

  18. Production rate & Spectrum • protons, dQ/dE~(1+z)mE-a • teff. : p + gCMB N +p Q=J/ teff. cteff [Mpc] log(E2dQ/dE) [erg/Mpc2 yr] GZK (CMB) suppression [Katz & EW 09] • Consistent with • protons, E2(dQ/dE) ~1043.7 erg/Mpc3 yr + GZK [EW 1995; Bahcall & EW 03]

  19. Back up slides

  20. Anisotropy Biased (rsource~rgal for rgal>rgal ) • Anisotropy @ 98% CL; Consistent with LSS (Correlation with low-luminosity AGN? Trace LSS) • Anisotropy/Compostion connection Acceleration of Z(>>1) to E  Acceleration of p to E/Z Anisotropy of Z @ E  Stronger anisotropy @ E/Z Anisotropy not observed @ E/Z  Z~1 @ E~1019.7eV [Kashti & Waxman 08] [:Lemoine & EW 09]

  21. & IceCube AMANDA

  22. The Mediterranean effort • ANTARES (NESTOR, NEMO) KM3NeT

  23. M82 M81 Mark Westmoquette (University College London), Jay Gallagher (University of Wisconsin-Madison), Linda Smith (University College London), WIYN//NSF, NASA/ESA Robert Gendler

  24. A lower bound: Star bursts • Star burst galaxies: - Star Formation Rate ~103Msun/yr >> 1 Msun/yr “normal” (MW) - Density ~103/cc >> 1/cc “normal” - B ~1 mG >> 1mG “normal” • Most stars formed in (z>1.5) star bursts • High density + B: CR e-’s lose all energy to synchrotron radiation CR p’s lose all energy to p production [Quataert et al. 06] [Loeb & Waxman 06]

  25. Starbursts Synchrotron radio Fn calibration p0gg, Fn ~Fg M82, NGC253: Hess, VERITAS 09 Fermi 09 dN/dE~1/Ep, p<~2.2 [Loeb & Waxman 06]

  26. The 1020eV challenge v R B /G v G2 G2 2R l =R/G (dtRF=R/Gc) [Waxman 95, 04, Norman et al. 95]

  27. The GRB “GZK sphere” g p • LSS filaments: D~1Mpc, fV~0.1, n~10-6cm-3, T~0.1keV eB=(B2/8p)/nT~0.01 (B~0.01mG), lB~10kpc • Prediction: D lB [Waxman 95; Miralda-Escude & Waxman 96, Waxman 04]

  28. GRB Model Predictions [Miralda-Escude & Waxman 96]

  29. Indirect detection J(>1011GeV)~1 / 100 km2 year 2p sr Auger: 3000 km2 3,000 km2 Fluorescence detector Ground array

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