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New Physics with 10 20 eV Neutrinos, and Advantages of Space-Based Observation

New Physics with 10 20 eV Neutrinos, and Advantages of Space-Based Observation. Tom Weiler Vanderbilt University. Cosmic Photon- Proton-Spectra. SN87a. sun. Neutrino Incognito. hadron wall?. no wall a’tall. CR Spectrum above a TeV. from Tom Gaisser. 50 Joules. VLHC (100 TeV) 2.

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New Physics with 10 20 eV Neutrinos, and Advantages of Space-Based Observation

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  1. New Physics with 1020 eV Neutrinos,andAdvantages of Space-Based Observation Tom Weiler Vanderbilt University Tom Weiler, Vanderbilt University

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

  3. CR Spectrum above a TeV from Tom Gaisser 50 Joules VLHC (100 TeV)2 Tom Weiler, Vanderbilt University

  4. 3 x1020 eV = macroscopic 50 Joules Clemens does this with 1027 nucleons; Nature does this with one nucleon, 1027 times better pitcher ! Tom Weiler, Vanderbilt University

  5. General Remarks on Neutrinos Existence of Xgal neutrinos inferred from CR spectrum, up to 1020 eV, and similarly, Galactic up to 1018 eV, Need gigaton (km3) mass (volume) for TeV to PeV detection [e.g. IceCube Xpt] but a teraton of mass at 1019 eV  SPACE-BASED [e.g. EUSO Xpt] Neutrino eyes see farther ( z>1 ), and deeper (into compact objects) than gamma-photons, and straighter than HECRs, with no absorption at (almost) any energy Tom Weiler, Vanderbilt University

  6. 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

  7. EE Neutrinos are young 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 millsec ! And it doesn’t even see the stream of radiation rushing past it – untouched ! Tom Weiler, Vanderbilt University

  8. Extreme Energy (EE) Neutrino Sources Bottom-Up “Zevatrons” - givens Cosmogenics ~1019 eV ·     AGNs ·     GRBs ·     Hidden vs. Transparent (the thick/thin debate) Top-Down “EE-trons” - pure speculation ·     Topological Defects ·     Wimpzillas, M ~H(post-inflation) ~1022 eV ·     Msee-saw ~ 1023 eV ·     MGUT ~ 1025 eV ·     And even MPlanck ~ 1028 eV Other: - impure thoughts   Mirror-Matter mixing Multiverse Leakage (Brane-bridges) Tom Weiler, Vanderbilt University

  9. Protheroe Summary Fluxes Cosmogenic n’s: Fn(Ep/5/4) = Fp(E>5 1019) x 20 Tom Weiler, Vanderbilt University

  10. In this biz, Size matters EUSO ~ 300 x AGASA ~ 15 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger Tom Weiler, Vanderbilt University

  11. 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

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

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

  14. Goldstone Lunar Radio (Cherenkov) Experiment (GLUE) GLUE is related to RICE, FORTE, and ANITA, and eventually, to Lofar and SalSa radio Cherenkov n Or better, a lunar orbiting antenna – “Moonita” Tom Weiler, Vanderbilt University

  15. Model Neutrino Fluxes and Future Limits GLUE, RICE, Forte ,Auger, Anita, EUSO From Eberle, AR, Song, TJW; Semikoz and Sigl Tom Weiler, Vanderbilt University

  16. Neutrino cross-section measurement Neutrinos at 1020 eV probe the structure of the nucleon at unprecedented small-x values ; Provides new QCD information CM energy at HERA is 0.3 TeV; while at En~ 1020 eV, Nature gives us Ecm ~ PeV! And so probes new thresholds, e.g. SUSY, X-Dimensions, TeV-scale Gravity, EW Instantons (NonPert. EW), … Reminder: LHC Ecm =14 TeV, and ILC Ecm =0.5 TeV Tom Weiler, Vanderbilt University

  17. n-N cross-section at 1020 eV Tom Weiler, Vanderbilt University

  18. Can’t Lose Thm for Space-based Whatever the weak cross-section, get robust event rate from HAS or UAS! and Get measurement of neutrino cross-section (peak angle also gives snN) A. Kusenko, TJW (PRL2002) Tom Weiler, Vanderbilt University

  19. Earth Absorption versus Neutrino Cross-Section ~ HERA value At Ecm=0.3 TeV Tom Weiler, Vanderbilt University

  20. Upward and Horizontal Air-shower Rates Versus Neutrino Cross-section HAS UAS Tom Weiler, Vanderbilt University

  21. Palomares-Ruiz, Irimia, TJW, Phys Rev D (2006), 33pp. solid lines are water, dashed lines are land Volume favors space-based over land-based by one or more orders of magnitude; for UAS, water also favors space-based by one or more orders of magnitude Tom Weiler, Vanderbilt University

  22. High-Energy Neutrino Astrophysics can be done only from Space Let’s do it ! Summary Tom Weiler, Vanderbilt University

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