1. Astrophysics of high energy cosmic-rays Eli Waxman Weizmann Institute, ISRAEL “New Physics”: talk by M. Drees Bhattacharjee & Sigl 2000

2. Cosmic ray flux and Composition E [GeV] log [dJ/dE] 110 610 E -2.7 E -3 Heavy Nuclei Protons Light Nuclei (p?) U cr (1GeV)=1 eV/cm 3 Galactic plane enhancement Isotropy Galactic X-Galactic [Blandford & Eichler, Phys. Rep. 87; Axford, ApJS 94; Nagano & Watson, Rev. Mod. Phys. 00]

3. Challenge I: Acceleration R B v v

4. Brightest known sources AGN jets (steady):  ~ few requires L>10 47 erg/s Few, brightest AGN GRBs (transient):  ~ 300 requires L>10 51 erg/s Average L  ~10 52 erg/s [Srittmatter 82 Biermann & Strittmatter 87] [Waxman 95; Vietri 95; Milgrom & Usov 95]

5. The Suspects losses 1/  [Hillas 84; Arisaka 02]

6. Comments on “ Magnetars ” Newborn Neutron stars (Hypothesis) with: B~10 14 G,  ~10 4 /sec L EM ~10 50 erg/s for t<1 min. Some difficulties: Wind should penetrate envelope with <10 -12 M sun entrainment Acceleration mechanism: Unknown NS ~1 M sun envelope EM wind [e.g. Blasi, Epstein, Olinto 00; Arons 02]

7. Challenge II: Propagation (GZK)  n (p) +(0)+(0) CMB p 10 100 1000 0.51.03.0 [Greisen 66; Zatsepin & Kuzmin 66]

8. Model Fly ’ s Eye fit for Galactic heavy (<10 19 eV): J G ~E -3.50 X-Galactic protons: Generation spectrum (shock acceleration): Generation rate (GRB motivated): Redshift evolution ~ SFR (GRB motivated). [Waxman 95]

9. The Data

10. Data- Calibrated at 10 19 eV

11. Model vs. Data X-G Model: [Bahcall & Waxman 02] Ruled out 7  55

12. Conclusions are Robust

13. Data/Model consistency Yakutsk, Fly ’ s Eye, HiRes: Consistent with XG protons: + GZK AGASA (25% of total exposure): Consistent below 10 20 eV Excess above 10 20 eV: 2.2+/-0.8 8 observed New source/New physics/ 25% energy Local inhomogeneity over-estimate Need: Large, hybrid 10 18 eV to 10 20 eV detector (Auger) ?

14. The Auger Observatory: 10 3.5 km 2 [Cronin 92, Watson 93]

15. Gamma-ray Bursts M on ~1 Solar Mass BH Relativistic Outflow e - acceleration in Collisionless shocks e - Synchrotron MeV  ’s L  ~10 52 erg/s  ~300 [Meszaros, ARA&A 02]

16. Proton/electron acceleration Protons Acceleration: Particle spectrum: p energy production: Electrons MeV  ’ s:  spectrum  energy production [Waxman 95] [Frail et al. 01 Schmidt 01]

17. GZK: Sources AGN, Radio-galaxies  GRBs : For R GRB (z=0)~0.5/Gpc 3 yr Prediction: p  D B [Schmidt 01] [Waxman 95, 01] [Miralda-Escude & Waxman 96]

18. GRBs: An illustrative example [Miralda-Escude & Waxman 96 ]

19. GRB Model Predictions <2x10 20 eV: Homogeneous + GZK >3x10 20 eV: Few, narrow spectrum sources Fluctuations (no homogeneous GZK) For more: Lec. Notes Phys. review (astro-ph/0103186)

20. “ Standard Model ” GRB ’ s Weak dependence on model parameters [Waxman & Bahcall 97, 99] [Rachen & Meszaros 98; Guetta, Spada & Waxman 01]

21. Diffuse Flux Bound Observed J CR (>10 19 eV) p  losses on CMB z<0.25 For Sources with   p <1: Strongest know z evolution (QSO, SFR): [Waxman & Bahcall 99, Bahcall & Waxman 01]

22.   p for known sources pp ’’ n ++ e+e+ e-e- 

23. Antares (0.1 Gton) Nemo (1 Gton) Anita (Radio, Balloon)

24. The AMANDA South-pole experiment

25. AMANDA neutrino event [Andres et al., Nature 01]

26. The Mediterranean ANTARES experiment

27. Summary Yakutsk, Fly ’ s Eye, HiRes: Consistent with GZK AGASA: >10 20 eV excess Main Challenge: Astrophysical accelerator physics Candidate: GRBs Hybrid, 10 3.5 km 2 Auger: GZK spectrum; Constraints on astro. sources UHE CRs High energy sources: 1--10 3 TeV: 1 km 3 (Optical Cerenkov) detectors Amanda, Antares, Nestor, IceCube, Nemo >>10 3 TeV: >>1 km 3 (Radio Cerenkov) detectors Anita, Rice

28. telescopes: some prospects GRB detection     appearance Lorentz Inv. (1-v/c : 10 -16 ), Weak equivalence principle (  L/c 3 : 10 -6 )