Controversy and Mystery in Highest-Energy Cosmic rays

1. Controversy and Mystery in Highest-Energy Cosmic rays • Tom Weiler • Vanderbilt University Tom Weiler, Vanderbilt University

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

3. The Cosmic Ray Timeline 1912 Hess (Austrian) balloons to 5km, his sparks increase; also sees no change during solar eclipse 1929 Cloud chambers, and the birth of particle physics: 1933 Anderson’s positron; Kunze’s muon (Rostock) 1937 Anderson’s muon 1938 Auger’s remarkable PeV air-shower 1949-54 Fermi’s “Doppler” acceleration via magnetized shocks 1966 3K CMB discovered; GZK predict cutoff at 5x1019 eV (But Linsley already reported (PRL) event at 1020 eV) 1987 IMB/Kamiokande neutrinos from SN87a Tom Weiler, Vanderbilt University

4. Auger, in 1938, separated two particle counters by a km high in the Swiss Alps (Jungfrau, near Bern), he discovered coincident signals. He calculated ETOT to be about 1015 eV. His inference was correct. His energy was 107 times the prior record event, And now thought to be typical of emission from a SN remnant. AUGER’s key discovery Cospar2004

5. 1991 Fly’s Eye reports 3x1020 eV, with proton-like profile; Akeno/AGASA Xpt begins  mid-90s DUMAND taken off life-support  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

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

7. 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

8. 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

9. 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

10. Size matters EUSO ~ 300 x AGASA ~ 10 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 events/year above 1020eV and UHE Neutrinos! 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 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. Xgal proton fit huge n flux low Xgal dominance flux, with no evolution WB fluxes AGHW 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

21. 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

22. 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 in prep.) Tom Weiler, Vanderbilt University

23. AMANDA to 100 TeV Tom Weiler, Vanderbilt University

24. “Essentially Guaranteed” Xgal n Flux HiRes 2004 fit: Green: galactic component Red: Xgal component Evolution parameter 2.8 +/- 0.3 Cosmogenic n’s: Fn(Ep/5/4) = Fp(E>5 1019) x 20 Tom Weiler, Vanderbilt University

25. “Essentially Guaranteed”Xgal Cosmogenic n Flux Cosmogenic n’s: Fn(Ep/5/4) = Fp(E>5 1019) x 20 graphs from Semikoz and Sigl Tom Weiler, Vanderbilt University

26. “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

27. “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

28. Relic Neutrino density – meV astrophysics Neutrino density from CMB density Tom Weiler, Vanderbilt University

29. Resonant Neutrino Annihilation Mean-Free-Path From Fargion, Mele, Salis l=(nn sn)-1 = 40 DH/h70 (neglecting higher densities at earlier times) Tom Weiler, Vanderbilt University

30. Escher’s Angels and Devils” Looking back, nn~(1+z)3, And so the absorption is greatly Enhanced for n’s from high-z sources Tom Weiler, Vanderbilt University

31. Neutrino mass-spectroscopy: absorption and emission The only possibility to directly infer the relic n density Tom Weiler, Vanderbilt University

32. zmax=2, 5, 20 (top to bottom), n-a=2 (bottom-up acceleration) Eberle, Ringwald, Song, TJW, 2004 n-mass spectroscopy Tom Weiler, Vanderbilt University

33. Z-bursts TJW, 1982; Revival – 1997 ~ 50 Mpc Tom Weiler, Vanderbilt University

34. 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