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Radio detection of UHE neutrinos

Radio detection of UHE neutrinos. E. Zas, USC Leeds July 23 rd 2004. J. Alavarez-Muñiz F. Halzen E. Marques T. Stanev R. Vazquez E. Zas. Contents:. Why UHE n? How does it work? What are the advantages? Which experiments ?. Neutrino - Cosmic Ray connection.

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Radio detection of UHE neutrinos

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  1. Radio detection of UHE neutrinos E. Zas, USC Leeds July 23rd 2004

  2. J. Alavarez-Muñiz F. Halzen E. Marques T. Stanev R. Vazquez E. Zas Contents: • Why UHE n? • How does it work? • What are the advantages? • Which experiments? Radio Detection

  3. Neutrino - Cosmic Ray connection • CR knwn to exist with E>1020 eV • UHECR mechanisms produce n • By fragmentation[“Top Down” Z-burst ...] • By interaction [Fermi] • With matter • With radiation Interactions with CMB => GZK neutrinos There must be UHE neutrinos! Radio Detection

  4. Acceleration Fragmentation p+g q q X p+ p0 p p : p0 : p+/- 0.03 : 0.3 : 0.65 p+p nm m+ nm ne e+ gg p p : n 1 : 6 p : g : n 0.09 : 2 : 6 ( ) ( ) g : nm :ne 2 : 4:2 The n / p flux ratio: A step towards UHECR source origin Radio Detection

  5. Target: The GZK n-spectrum • GZK neutrino flux depends on: • Cosmic Ray spectrum • Source distribution • Maximum redshift • Source evolution Radio Detection

  6. ____ ____ ____ ONE source only Uniform Distribution UD + strong evolution E-2 p-spectrum after CMB interactions CR Flux / Reference Flux D.Gonzalez,RAV,EZ (in prep) Radio Detection

  7. E-2 _________ U Dis+evol _________ Unif Distr _________ one source CR Flux / Reference Flux D.Gonzalez,RAV,EZ (in prep) Radio Detection

  8. E-2 _________ U Dis+evol _________ Unif Distr _________ one source P & n-Flux / Reference Flux D.Gonzalez,RAV,EZ (in prep) Radio Detection

  9. Radio wavelength (l)> Emission length w l Coherent Radiation Radio pulses from showers: Why? • SIGNAL POWER • Electric Field ~ Q • STABILITY • To shower fluctuations • INFORMATION • Spatial distribution • Frequency Spectrum Radio Detection

  10. Cherenkov in radio (Askary’an 1960) Wavelength(l) >>l,we- and e+ cancel !! But what about excess Ne--Ne+? • e,g interactions have charge symmetry • But matter only has electrons!! • Interaction with matter electrons • Askary’an predicted ~10% charge excess Radio Detection

  11. e+ g e- e- Compton e+ e+ e- e- e- e- media electrons Bhabha Möller Processes contributing to the excess charge Annihilation Radio Detection

  12. ICE ZHS:FH,TS,EZ, PRD(91) Radio Detection

  13. if w=0 or q=qc or dt=0 tracklength Calculate radio pulse interference (Fraunhofer limit) Radio Detection

  14. Radio Detection

  15. Radio Detection

  16. |E| a Ne-Ne+ Scaling Ne-Ne+a ESHOW Signal Power Radio Pulse Power a|E|2a E2SHOW Radio Detection

  17. Radio Detection

  18. Radio Detection

  19. Radio Detection

  20. Radio Detection

  21. Kind of FT with The slit diffraction analogy If current is “thin”: Radio Detection

  22. qc Stability (because k=0) Radio Detection

  23. Calculations of UHE with hybrid code with LPM effect!! • Electromagnetic showers Dq~E-1/3 above 10 PeV • Hadronic Showers hardly any elongation up to 100 EeV • n showers measure y? Radio Detection

  24. Radio Detection

  25. Radio Detection

  26. Radio Detection

  27. Natural transparent media ICE: Antarctica RICE (array buried) ANITA (balloon) Greenland FORTE (satellite) SALT: Domes explored SALSA MOON REGOLITH: Radiotelescopes GLUE Radiotelecope array LUNASKA (ska) ATMOSPHERE: Antenna array LOFAR Coherent radio detection: n-experiments Radio Detection

  28. Askary’an effect confirmed: SLAC P.Gorham, D.Saltzberg et al. PRL (2000) Radio Detection

  29. Radio Detection

  30. Coherence! |E| a Esh |E(w)| spectral agreement Radio Detection

  31. Radio Technique has an enormous potential To detect highest energy events To get detail about showers To cover large surfaces There are many projects under consideration It is worth pursuing them It is likely that radio provides the next step in the search for UHE radiation Summary and conclusion: Radio Detection

  32. Both Cosmic Ray & n-detector Different geometries CR n Radio Detection

  33. Radio Detection

  34. MOON JAlvarez Muñiz Complex acceptance geometry Radio Detection

  35. Radio Detection

  36. FORTE low frequency search system for transients Lehtinen, PG et al. astro-ph/0309656 (weather measurements) central n:20-300 MHz bandwith: 22 MHz 5 subbands coincidences Data Sep 97-Dec 99 2003 BOUND Radio Detection

  37. Radio Detection

  38. Radio Detection P. Gorham, et al. astro-ph/0310232

  39. Radio Detection

  40. E-2 _________ U Dis+evol _________ Unif Distr _________ one source GZK n-Flux D.Gonzalez,RAV,EZ (in prep) Radio Detection

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