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Lepton - Photon 01 Francis Halzen

Lepton - Photon 01 Francis Halzen. the sky > 10 GeV photon energy < 10 -14 cm wavelength > 10 8 TeV particles exist Fly’s Eye/Hires they should not more/better data arrays of air Cherenkov telescopes 10 4 km 2 air shower arrays ~ km 3 neutrino detectors. Energy (eV ).

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Lepton - Photon 01 Francis Halzen

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  1. Lepton - Photon 01Francis Halzen the sky > 10 GeV photon energy < 10-14 cm wavelength > 108 TeV particles exist Fly’s Eye/Hires they should not more/better data arrays of air Cherenkov telescopes 104 km2 air shower arrays ~ km3 neutrino detectors

  2. Energy (eV) 1 TeV Radio CMB Visibe GeV g-rays Flux

  3. n / / / / / / / / / / / / / / / / / TeV sources! cosmic rays

  4. With103 TeV energy, photons do not reach us from the edge of our galaxy because of their small mean free path in the microwave background. g + g e++ e-

  5. fluorescence from atmospheric nitrogen + _ cosmic ray + _ o  fluorescent light electromagnetic shower

  6. Acceleration to 1021eV? ~102 Joules ~ 0.01 MGUT • dense regions with exceptional • gravitational force creating relativistic • flows of charged particles, e.g. • annihilating black holes/neutron stars • dense cores of exploding stars • supermassive black holes

  7. Cosmic Accelerators E ~ GcBR R ~ GM/c2 magnetic field energy E ~GBM mass boost factor

  8. E > 1019 eV ? E ~ GB M > ~ quasars G @ 1 B @ 103G M @109 Msun blasarsG 10 neutron stars G@ 1B @ 1012G M @ Msun black holes . . grbG102 > ~ emit highest energy g’s!

  9. Profile of Gamma Ray Bursts • Total energy: one solar mass • Photon energy: 0.1 MeV to TeV • Duration: 0.1 secs -- 20 min • Several per day • Brightest object in the sky • Complicated temporal structure: no ‘typical’ burst profile

  10. A few more results … • Gamma Ray Bursts (GRBs) • Observation of single 3 s excess (GRB 970417a) within 1997 BATSE trigger. • Flux limit for unidentified TeV point sources • For E spectrum Flux (>1 TeV) < 2 – 30 x 10-7 cm-2 s-1 @90% AMANDA II will probe this flux for n/g = 1 However, g spectrum probably softer due to reprocessing (core) and absorption in photon BG

  11. Particles > 1020 eV ? • not protons • cannot reach us from cosmic accelerators • lint < 50 Mpc • no diffusion in magnetic fields • doublets, triplet • not photons • g + Bearth e+ + e- not seen • showers not muon-poor • not neutrinos • snp 10-5spp no air showers

  12. Interaction length of protons in microwave backgroundp + gCMBp + …. lgp = (nCMBs  ) -1 @10 Mpc p+gCMB GZK cutoff

  13. Forthcoming AGASA Results • The highest energy cosmic rays do come from point sources: 5 sigma correlation between directions of pairs of particles. Birth of proton astronomy! • Are the highest energy cosmic rays Fe? GKZ cutoff at ~2 1020 eV ?

  14. Particles > 1020 eV ? new astrophysics? • not protons • cannot reach us from cosmic accelerators • lint < 50 Mpc • no diffusion in magnetic fields • doublets, triplet • not photons • g+ Bearth e+ + e- not seen • showers not muon-poor • not neutrinos • snp10-5spp no air showers trouble for top-down scenarios sn p@ spp with TeV - gravity unitarity?

  15. _ 1024 eV = 1015 GeV ~ MGUT are cosmic rays the decay product of • topological defects • (vibrating string, annihilating monopoles) • heavy relics? Top. Def.  X,Y  W, Z  quark + leptons  >> p   g • top-down spectrum • hierarchy n  g p

  16. black hole radiation enveloping black hole

  17. cosmic ray puzzle neutrinos protons TeV g - rays ~ 1 km3 high energy detectors ~ 104 km2 air shower arrays • atmospheric Cherenkov • space-based • AMANDA / Ice Cube • Antares, Nestor, • NEMO • Veritas, Hess, Magic … • GLAST… • Hi Res, Auger, • Airwatch, • OWL, TA… e.g. • particle physics • and cosmology • dark matter search • discovery • short-wavelength • study of supernova • remnants and galaxies also

  18. Array => Very large effective area (105 m2) => 3-dim shower reconstruction => Dramatic improvements in - Energy Resolution - Background Rejection

  19. STACEE Solar Tower Atmospheric Cherenkov Effect Experiment Gamma-ray Astrophysics between 50-500 GeV

  20. ne+ e W m+ nm 6400 TeV

  21. nt t PeVt(300m) t decays

  22. Why is Searching forn’s from GRBs of Interest? • Search for vacuum oscillations (nnt): • Dm2  10-17 eV2 • Test weak equivalence principle:10-6 • Test : 10-16 > ~ Cphoton - Cn Cn

  23. Lepton - Photon 01Francis Halzen the sky > 10 GeV photon energy < 10-14 cm wavelength > 108 TeV particles exist Fly’s Eye/Hires they should not more/better data arrays of air Cherenkov telescopes 104 km2 air shower arrays ~ km3 neutrino detectors

  24. n / / / / / / / / / / / / / / / / / TeV sources! cosmic rays

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