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Lecture on Cosmic Neutrino Factory

Lecture on Cosmic Neutrino Factory. Cosmic Neutrino Factory. black hole. radiation enveloping black hole. p + g -> n + p + ~ cosmic ray + neutrino. -> p + p 0 ~ cosmic ray + gamma. W-B Bound. Evading the Bound.

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Lecture on Cosmic Neutrino Factory

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  1. Lecture on Cosmic Neutrino Factory www.assignmentpoint.com

  2. Cosmic Neutrino Factory black hole radiation enveloping black hole p + g -> n + p+ ~ cosmic ray + neutrino -> p + p0 ~ cosmic ray + gamma www.assignmentpoint.com

  3. W-B Bound www.assignmentpoint.com

  4. Evading the Bound • “Neutrino only” sources that are optically thick to proton photo-meson interactions and from which protons cannot escape. • No observational evidence (from baryons or high energy photons) • Cores of AGNs (rather than in the jets) by photo-meson interactions or via p−p collisions in a collapsing galactic nucleus or in a cacooned black hole. • The most optimistic predictions of the AGN core model have already been ruled out by AMANDA www.assignmentpoint.com

  5. Mannheim, Protheore and Rachen Model www.assignmentpoint.com

  6. Neutrinos from Cosmic Rays ~50 events/km2/yr www.assignmentpoint.com

  7. Size Perspective for KM3 AMANDAII 300 m 1500 m 50 m 2500 m www.assignmentpoint.com

  8. Detection Technique Cerenkov light cone muon or tau interaction detector See Talks in this Session • The muon radiates blue light in its wake neutrino • Optical sensors capture (and map) the light www.assignmentpoint.com

  9. Electromagnetic and hadronic cascades ~ 5 m Detection ofe, , O(km) long muon tracks  17 m direction determination by cherenkov light timing www.assignmentpoint.com

  10. Muon Events Eµ= 6 PeV Eµ= 10 TeV Measure energy by counting the number of fired PMT. (This is a very simple but robust method) www.assignmentpoint.com

  11. Determining Energy 6 PeV m 10 TeV m 375 TeV Cascade www.assignmentpoint.com

  12. t + N --> t- + X t + X (82%) Double Bang Learned, Pakvasa, 1995 Regeneration makes Earth quasi transparent for high energie ; (Halzen, Salzberg 1998, …) Also enhanced muon flux due to Secondary µ, and nµ (Beacom et al.., astro/ph 0111482) E << 1PeV: Single cascade (2 cascades coincide) E ≈ 1PeV: Double bang E >> 1 PeV: partially contained (reconstruct incoming tau track and cascade from decay) www.assignmentpoint.com

  13. Tau Cascades E << 1PeV: Single cascade (2 cascades coincide) E ≈ 1PeV: Double bang E >> 1 PeV: partially contained (reconstruct incoming tau track and cascade from decay) www.assignmentpoint.com

  14. Neutrino ID (solid)Energy and angle (shaded) Neutrino flavor www.assignmentpoint.com

  15. Tau Transparency/Regeneration • ne and nµ are absorbed in the Earth via charged current interactions (muons range out) • Above ~100 TeV the Earth is opaque to ne & νµ. • But, the Earth never becomes completely opaque to nt • Due to the short t lifetime, t’s produced in nt charged-current interactions decay back into nt • Also, secondary ne & νµ. fluxes are produced in the tau decays. www.assignmentpoint.com

  16. Flavor Ratios • The ratio of flavors at the source is expected to be 0:2:1= nt : nm : ne • Since the distance to the source is >> than the oscillation length – any admixture at the source should wind up: 1:1:1= nt : nm : ne when arriving at earth • What if that isn’t true? www.assignmentpoint.com

  17. Exotic neutrino properties if not 1:1:1 • Neutrino decay (Beacom, Bell, Hooper, Pakvasa& Weiler) • CPT violation (Barenboim& Quigg) • Oscillation to steriles with very tiny delta δm2 (Crocker et al; Berezinskyet al.) • Pseudo-Dirac mixing (Beacom, Bell, Hooper, Learned, Pakvasa& Weiler) • 3+1 or 2+2 models with sterile neutrinos (Dutta, Reno and Sarcevic) • Magnetic moment transitions (Enqvist, Keränen, Maalampi) • Varying mass neutrinos (Fardon, Nelson & Weiner; Hung & Pas) www.assignmentpoint.com

  18. Count rates 0 5 10 sec Supernova Monitor B10: 60% of Galaxy A-II: 95% of Galaxy IceCube: up to LMC Amanda-II Amanda-B10 IceCube www.assignmentpoint.com

  19. Large Scale Neutrino Detectors ANTARES La-Seyne-sur-Mer, France BAIKAL Russia NEMO Catania, Italy See Talks in this Session NESTOR Pylos, Greece IceCube, South Pole, Antarctica www.assignmentpoint.com

  20. Radio Cherenkov Detectors Rice Anita Salsa www.assignmentpoint.com

  21. Acoustic Detectors SAUND(Study of Acoustic Underwater Neutrino Detection) www.assignmentpoint.com

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