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UHECRs & GRBs

UHECRs & GRBs. Eli Waxman Weizmann Institute, ISRAEL. The acceleration challenge. v. R. /G. B. v. 2R. G 2. G 2. l =R/ G. (d t RF =R/ G c). [Hillas, ARA&A (1984); Waxman 04]. The suspects. Active Galactic Nuclei (steady): G ~ few requires L>10 47 erg/s Few, brightest AGN

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UHECRs & GRBs

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  1. UHECRs & GRBs Eli Waxman Weizmann Institute, ISRAEL

  2. The acceleration challenge v R /G B v 2R G2 G2 l =R/G (dtRF=R/Gc) [Hillas, ARA&A (1984); Waxman 04]

  3. The suspects • Active Galactic Nuclei (steady): G~ few requires L>1047 erg/s Few, brightest AGN • Gamma Ray Bursts (transient): G~ 300 requires L>1051 erg/s Average Lg~1052 erg/s

  4. The Suspects losses 1/b [Hillas 84; Arisaka 02]

  5. Comments on “Magnetars” • Newborn Neutron stars (Hypothesis) with: B~1014G, W~104/sec LEM~1050 erg/s for t<1 min. • Some difficulties: Wind should penetrate envelope with <10-12 Msun entrainment Acceleration mechanism: Unknown [e.g. Blasi, Epstein, Olinto 00; Arons 02] EM wind NS ~1 Msun envelope [Waxman 04]

  6. Gamma-ray Bursts M on ~1 Solar Mass BH Relativistic Outflow e- acceleration in Collisionless shocks G~300 MeV g’s: Lg~1052erg/s UHE p Acceleration e-Synchrotron X-ray, UV Radio [Piran, Phys. Rep. 99; Meszaros, ARA&A 02; Waxman, Lec. Notes Phys. 598 (2003).]

  7. Protons Acceleration/expansion: Synchrotron losses: Particle spectrum: p energy production: Electrons MeV g’s: Optical depth: g spectrum: g energy production Proton/electron acceleration: ‘95 [Waxman 95, PRL 75, 386; ApJ 452, L1; Note: Constraints independent of details of acceleratiomn model (e.g. Gialis & Pelletier 04)]

  8. 1997: BeppoSAX (GRB afterglows) • Detection of (predicted) X-ray, Optical & Radio “afterglow” • Identification of “host” galaxies, <z>~2 • Detailed tests of the model Size measurements [scintillation, VLBI, sub-rel.] X-ray to radio (synchrotron) spectra [e.g. Meszaros, ARA&A 02] [Waxman, Kulkarni & Frail 98; Taylor, Frail, Berger & Kulkarni 04; Frail, Waxman & Kulkarni 00; Berger, Kulkarni & Frail04] [e.g. 970508, Wijers & Galama 98]

  9. Afterglow: UHECR implications • Lg=1051 erg/s -> Lg=1052 erg/s • Early optical afterglow: uB/ue~1, G~102.5 • Revised rates, energy 10/Gpc3yr -> 0.5/Gpc3yr Eg=1052 erg -> Eg=1053.5 erg [Zhang,Kobayashi, Meszaros 03; Soderberg, Ramirez-Ruiz 03] [Schmidt 01; Guetta, Piran, Waxman 03]

  10. Protons Acceleration/expansion: Synchrotron losses: Particle spectrum: p energy production: Electrons MeV g’s: Optical depth: g spectrum: g energy production Proton/electron acceleration Afterglow 0.02 52 [Waxman 95] [Waxman 04]

  11. UHECR generation ~1019eV [Watson 91, Nagano & Watson 00] • Galactic heavy nuclei X-Galactic protons • X-Galactic protons Generation spectrum & rate (z evolution follows SFR): • <1019eV Galactic heavy nuclei Fly’s Eye fit: JG~E-3.50 [Waxman 95; Bahcall & Waxman 03]

  12. Model vs. Data Ruled out at 5s [Bahcall & Waxman 03]

  13. “GZK sphere” g • AGN, Radio-galaxies  • GRBs  : • For RGRB(z=0)~0.5/Gpc3yr • Prediction: p D lB [Waxman 95; Miralda-Escude & Waxman 96, Waxman 03]

  14. GRB Model Predictions • >3x1020eV: Few, narrow spectrum sources; Fluctuations (no homogeneous GZK). • Auger • AGASA multiplets- statistical significance? [Watson 91, Cronin 93] [Miralda-Escude & Waxman 96] [Teshima 03; Finley & Westerhoff 04]

  15. “Generic” GRB n’s Weak dependence on model parameters [Waxman & Bahcall 97, 99; Rachen & Meszaros 98; Alvarez-Muniz & F. Halzen 99; Guetta, Spada & Waxman 01; Guetta, Hooper, Alvarez-Muniz, Halzen & E. Reuveni 04]

  16. Summary • GRBs >1019eV protons (acceleration, rate) Predictions 103km2 area detectors experiments: HiRes, Auger, T.A., EUSO/OWL • GRBs 100TeV n’s Flux 1Gton detectors Experiments: Baikal, AMANDA IceCube, Antares, Nestor, NEMO • n detection GRBs: CR puzzle, GRB progenitors & physics n physics: nm ntt appearance Lorentz Inv. (10-16), Weak equivalence principle (10-6)

  17. Direct size measurement: Scintillation q q d > l d l h • Finite size, cosmological source: hcrit.~few x 1017cm dne Diffractive scintillation [Frail, Waxman & Kulkarni 00]

  18. “Cannon balls” • Proper motion: D&D 2003: >1.4 mas for 030329 Obs.: 0.1+-0.1 • Inconsistent with scintillation suppression [ Dado, Dar & De Rujula 02]

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