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High-Energy Neutrino Astrophysics

High-Energy Neutrino Astrophysics. Tom Weiler Vanderbilt University. Neutrinos and the Early Universe”, Trento ECT* Workshop, October 4-8 2004. Cosmic Photo- Proto-Spectra. SN87a. sun. Neutrino Incognito. hadron wall?. no wall a’tall.

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High-Energy Neutrino Astrophysics

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  1. High-Energy Neutrino Astrophysics • Tom Weiler • Vanderbilt University Neutrinos and the Early Universe”, Trento ECT* Workshop, October 4-8 2004 Tom Weiler, Vanderbilt University

  2. Cosmic Photo- Proto-Spectra SN87a sun Neutrino Incognito hadron wall? no wall a’tall Tom Weiler, Vanderbilt University

  3. 1991 Fly’s Eye reports 3x1020 eV, with proton-like profile; Akeno/AGASA Xpt begins  mid-90s DUMAND taken off life-support; Baikal continues  90s SuperK neutrinos from the sun (directional astro)  1996 AGASA reports event clustering within 2.50 ang. res’n and: F(E  1020 eV) ~ 1/km2/century, withshower diameter ~ 5km, N(e) ~ 1011  2000 20 events at and above 1020 eV  2001 HiRes withdraws 7 events;AGASA adds 6 (from z > 45o); And the controversy has begun! Importantly, Auger gets first “light”  2002 AMANDA pushes to 1014 eV thru-Earth neutrinos   2005 Auger Observatory data expected  2008 Extreme Universe Space Observatory (EUSO) ? Tom Weiler, Vanderbilt University

  4. CR Spectrum above a TeV from Tom Gaisser VLHC (100 TeV)2 Tom Weiler, Vanderbilt University

  5. Highest Energy Event The CR record energy is 3x1020 eV (0.3 ZeV). Found by Fly’s Eye a decade ago (they got lucky!). This is truly a macroscopic energy: 3x1020 eV = 50 Joules equivalent to a Roger Clemens fastball, a Tiger Woods tee shot, a Pete Sampras tennis serve, Or a speeding bullet. (Also to 12 Calories, which heats a gram of water by 12oC) Tom Weiler, Vanderbilt University

  6. 3 x1020 eV = macroscopic 50 Joules Clemens does this with 1027 nucleons; Nature does this with one nucleon, 1027 times more efficient ! Tom Weiler, Vanderbilt University

  7. Fly’s Eye 3x1020 eV event (1992) 100 billion e+e- pairs at xmax ~ 800 g/cm2 This longitudinal profile is consistent with a primary proton, but not with a primary photon; Disfavors “local” top-down sources such as massive Particle DK, topo-defects, Z-bursts, etc. Tom Weiler, Vanderbilt University

  8. EE Neutrinos are young Liberated at T=Mev, t= 1 sec Depends on energy (Lorentz boost) Consider a 1020 eV neutrino. Lorentz factor = 1021 for mn = 0.1 eV. Age of Uni is 1018 sec, But age of n is 1018/1021 sec = 1 millisecond ! And it doesn’t even see the stream of radiation rushing past it – untouched ! Tom Weiler, Vanderbilt University

  9. Size matters EUSO ~ 300 x AGASA ~ 10 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger Tom Weiler, Vanderbilt University

  10. Article Images Extreme Universe Space Observatory • EUSO onboard the ISS (Or Not!) • 2012 Hundredth anniversary of Hess • – EUSO finishes three-year data-taking Tom Weiler, Vanderbilt University

  11. “clear moonless nights” Or New York State power blackout Tom Weiler, Vanderbilt University

  12. Orbiting Wide-angle Lens (OWL) 3000 events/year above 1020eV and UHE Neutrinos! Tom Weiler, Vanderbilt University

  13. nHAS event rate is small e.g. FCR at 1020 eV implies 10-2 events/yr; Tom Weiler, Vanderbilt University

  14. AGASA Spectrum: EeV to ZeV AGASA, July 2002 Tom Weiler, Vanderbilt University

  15. -resonance multi-pions Greisen-Zatsepin-Kuzmin and the Cosmic-Ray Wall Photo-pion production off CMB p+cmb  p/n+ Tom Weiler, Vanderbilt University

  16. HiRes vs. AGASA UHE spectrum FlysEye event goes here discovery opportunity GZK recovery ? Z-burst uncovery ? EUSO reach x 103 better Tom Weiler, Vanderbilt University

  17. AGASA hot-spots -- Data red: E > 4 1019 eV green: E > 1020 eV Cluster Component ~ E -1.8±0.5 Neutrinos will point better Tom Weiler, Vanderbilt University

  18. AGASA hot-spots -- numbers Within 2.5 degree circles, AGASA identifies six doublet, one triplet, Out of 57 events; Opening the angle to just 2.6 degrees, AGASA identifies seven doublets, two triplets; Haverah Park contributes two more paired events in AGASA directions. NOT corroborated by HiRes. • Source number ~ N12/2N2 ~ 270 to 50%, • weighting with GZK suppression, • ~ 10-5 /Mpc3for source density Tom Weiler, Vanderbilt University

  19. Berezinsky et al Xgal proton flux Mass-composition data (HiRes 2002) Theory threshold for pg2.7Kpe+e- and data (knee) are at 1017.6 eV. • Xgal proton dominance • begins at 1018 eV, not 1019 eV ! • Fn ~ 50 x Waxman-Bahcall • AMANDA/RICE/EAS-sensitive !! (AGHW, to appear) Tom Weiler, Vanderbilt University

  20. AMANDA to 100 TeV Tom Weiler, Vanderbilt University

  21. AMANDA/IceCube nm event Tom Weiler, Vanderbilt University

  22. Xgal proton fit huge n flux low Xgal dominance flux, with no evolution WB fluxes AGHW, hep-ph/04010003 xp is pion energy/CR energy at source (1 for WB “limit”); xz is cosmic evolution factor, 0.6 (no) to 3.0 (SFR) Tom Weiler, Vanderbilt University

  23. Neutrinos versusCosmic-Rays and Photons ns come from central engines - near Rs of massive BHs - even from dense “hidden” sources cf. ns vs. gs from the sun ns not affected by cosmic radiation (except for annihilation resonance) ns not bent by magnetic fields - enables neutrino astronomy Also, besides Energy and Direction, n’s carry flavor Tom Weiler, Vanderbilt University

  24. n diagnostic of astro-engines:ppp vs. pg p The process ne+e-- W-- is resonant at 6.4 PeV; IceCube will have flavor ID, and DE/E of 25%, and so can measure On-Res/Off-Res ratio. pp make nearly equal p+p-  nm:nm:ne:ne = 2:2:1:1  flavor democracy, ne = 1/6 total pg via D+ make p+  nm:nm:ne = 1:1:1 (no ne)  ne = 1/15 total IceCube can resolve this (AGHW, ArXiv this week) Tom Weiler, Vanderbilt University

  25. Flavor ratio  Topology ratio Map Beacom, Bell, Hooper, Pakvasa, TJW, 2003 Tom Weiler, Vanderbilt University

  26. The cosmicnflavor-mixing theorem If theta32 is maximal (it is), And if Re(Ue3) is minimal (it is), Then nm and nt equilibrate; Further, if initial ne flux is 1/3 (as from pion-muon decay chain), Then all three flavors equilibrate. ne:nm:nt = 1 : 1 : 1 at Earth Tom Weiler, Vanderbilt University

  27. Democracy Broken: • 1. n decay (15 minutes of fame) • 2. Vacuum resonance • (MaVaNs, LIV vector) • 3. Pseudo-Dirac n oscillations • 4. Source dynamics (w/ Farzan) Tom Weiler, Vanderbilt University

  28. Neutrino Decay -- Models, Signatures, and Reach Tom Weiler, Vanderbilt University

  29. “Essentially Guaranteed” High-Energy Galactic Neutrino Flux ctn = 10 kpc (En / EeV) and En/ En ~ Q / mn ~ 0.8 x 10-3  En ~ PeV, for En ~ EeV Tom Weiler, Vanderbilt University

  30. “More Guaranteed” Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher ! Icecube atmos background in 1o circle is just 1.5events/yr,  3.5 events offers 95% CL detection in 1 yr; Calculated signal is 4 nm /yr and 16 ne+nt showers/yr. Conclude that in a few years, IceCube attains 5s discovery sensitivity for Fe  n  ne  nm, Providing “smoking ice” for GP neutron hypothesis. Tom Weiler, Vanderbilt University

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