1 / 57

Neutrino Astrophysics: PeV to ZeV (with some whacky particle physics)

Neutrino Astrophysics: PeV to ZeV (with some whacky particle physics). Tom Weiler -- Vanderbilt University & CERN *. For the viewing pleasure of Alan, the only person to make me regret that I don’t play (cough) golf!. * thanks Alan, and Francis.

alanna
Download Presentation

Neutrino Astrophysics: PeV to ZeV (with some whacky particle physics)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Neutrino Astrophysics: PeV to ZeV(with some whacky particle physics) • Tom Weiler • -- Vanderbilt University & CERN* For the viewing pleasure of Alan, the only person to make me regret that I don’t play (cough) golf! * thanks Alan, and Francis Tom Weiler, Vanderbilt & CERN

  2. 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 Tom Weiler, Vanderbilt & CERN

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

  4. 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” - ?? ·     Topological Defects ·     Wimpzillas, M ~H(post-inflation) ~1022 eV ·     Msee-saw ~ 1023 eV ·     MGUT ~ 1025 eV ·     And even MPlanck ~ 1028 eV Other: - ????   Mirror-Matter mixing Multiverse Leakage Tom Weiler, Vanderbilt & CERN

  5. HiRes vs. AGASA UHE spectrum FlysEye event goes here discovery opportunity GZK recovery ? Z-burst discovery ? EUSO reach x 103 Tom Weiler, Vanderbilt & CERN

  6. nHAS event rate Tom Weiler, Vanderbilt & CERN

  7. Size matters EUSO ~ 300 x AGASA ~ 10 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger Tom Weiler, Vanderbilt & CERN

  8. “clear moonless nights” Tom Weiler, Vanderbilt & CERN

  9. “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 & CERN

  10. for comparison, AGN and Z-burst fluxes an AGN prediction and Z-burst fit Tom Weiler, Vanderbilt & CERN

  11. Present and Imminent Limits on Neutrino Flux Tom Weiler, Vanderbilt & CERN

  12. Model Neutrino Fluxes and Future Limits Eberle, Ringwald, Song, TJW Tom Weiler, Vanderbilt & CERN

  13. 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 & CERN

  14. Resonant Neutrino Annihilation Mean-Free-Path From Fargion, Mele, Salis l=(nn sn)-1 = 40 DH/h70 Tom Weiler, Vanderbilt & CERN

  15. Escher’s Angels and Devils” Tom Weiler, Vanderbilt & CERN

  16. Z-bursts TJW, 1982; Revival – 1997 ~ 50 Mpc Tom Weiler, Vanderbilt & CERN

  17. Neutrino mass-spectroscopy: absorption and emission Tom Weiler, Vanderbilt & CERN

  18. It “probably” looks something like this m3 Dm223 ~ 2.5 x 10-3 eV2 m2 Dm212 ~ 7 x 10-5 eV2 m1 nm ne nt What we think we know about neutrino mass Log m2 Tom Weiler, Vanderbilt & CERN

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

  20. Dips & sobering realism • hidden MX=4 1014 and 1016 GeV, • to explain >GZK w/ Z-bursts; • mass = 0.2 (0.4) eV - dashed (solid); Error bars – per energy decade, by 2013, for flux saturating present limits Tom Weiler, Vanderbilt & CERN

  21. Fitted Z-burst (Emission) Flux Gelmini, Varieschi, TJW Tom Weiler, Vanderbilt & CERN

  22. Nu-mass limit for Z-burst fitted to EECRs Gelmini, Varieschi, TJW Tom Weiler, Vanderbilt & CERN

  23. Neutrino Mass tomography in the Local Super-galactic Cluster (Fodor, Katz, Ringwald) Tom Weiler, Vanderbilt & CERN

  24. Upward and Horizontal Air-shower Rates Versus Neutrino Cross-section Kusenko, TJW HAS UAS Tom Weiler, Vanderbilt & CERN

  25. Earth Absorption versus Neutrino Cross-Section Tom Weiler, Vanderbilt & CERN

  26. Can’t Lose Thm 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) Kusenko, TJW hep-ph/ Tom Weiler, Vanderbilt & CERN

  27. The “Learned Plot” Oscillation phase is . ( L dm2 / 4 En ) Figure parameterized by dm2 / (eV)2 Tom Weiler, Vanderbilt & CERN

  28. Neutrino Decay -- Models, Signatures, and Reach P(survive)= e –t/t = e –(L/E)(m/t0) Beacom, Bell, Hooper, Pakvasa, TJW Tom Weiler, Vanderbilt & CERN

  29. PMNS neutrino-mixing matrix Weak-interaction and mass “vectors” point differently: |nk>=Uki |ni>, or Uki = <ni | nk> = <nk | ni>* Tom Weiler, Vanderbilt & CERN

  30. The cosmicnflavor-mixing thm 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 & CERN

  31. AMANDA/IceCube nm event Tom Weiler, Vanderbilt & CERN

  32. Flavor ratio  Topology ratio Map Tom Weiler, Vanderbilt & CERN

  33. Sensitivity of n1 flavor-projection to MNS parameters Tom Weiler, Vanderbilt & CERN

  34. Final “remark”:Is anyone driving to/by Nottingham East Midlands airport tomorrow morning?I could use a ride.Thank you. Tom Weiler, Vanderbilt & CERN

  35. 1991 Fly’s Eye reports 3x1020 eV, with proton-like profile; Akeno/AGASA Xpt begins 1993 Baikal sees underwater neutrinos  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 expected to go public Tom Weiler, Vanderbilt & CERN

  36. CR Spectrum above a TeV from Tom Gaisser VLHC (100 TeV)2 Tom Weiler, Vanderbilt & CERN

  37. Hillas Plot -- coherence length= B x L Tom Weiler, Vanderbilt & CERN

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

  39. WINDOWS on the UNIVERSE Crab Nebula Stars & Galaxies Galaxy Clusters Big Bang Planets Black Holes Neutron Stars Distant Galaxies Gamma Ray Bursts 10-3 1 103 106 109 1012 Limited Vision E L E C T R O M A G N E T I C S P E C T R U M Radio -wave IR /Visible/ UV X-rays -rays VHE -rays Accelerators Reactors, Nuclear Decays N E U T R I N O S P E C T R U M 10-3 1 103 106 109 1012 1015 1018 1021eV Sun Crab Nebula Produced by New Particles Atmospheric Neutrinos Big Bang Stars Dark Matter Produced by Ultra-High-Energy Cosmic Rays Neutron Stars Supermassive Black Holes Supernovae Gamma Ray Bursts Underground Lab IceCube Auger EUSO radio From Turner & Olinto Tom Weiler, Vanderbilt & CERN

  40. EUSO • Hundredth anniversary of V. Hess • – EUSO finishes three-year data-taking FOV = 2 105 km2, Aperture = 106 km2 sr, and 2 teratons of visible mass Tom Weiler, Vanderbilt & CERN

  41. “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 Anchordoqui, Goldberg, Halzen, TJW; hep-ph/0311002 Tom Weiler, Vanderbilt & CERN

  42. “More Guaranteed” Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher ! a signal in a km3. So, 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 & CERN

  43. Schematic: AGN Unified Source Model • annotated by M. Voit Tom Weiler, Vanderbilt & CERN

  44. The TeV g-ray -- PeV n connection A handful of TeV g-ray emitters have been identified, all of the BL-Lac class, with a relativistic jet slightly off-set from the line of sight. Two principle production mechanisms: Electrons: synchrotron on magnetic field, or inverse Compton on gamma’s; Hadrons: pion production off g’s and nucleons, with p0  g g (and p+/-  2 nm+ ne + e ) Only the latter accommodates production of observed CRs ! In the Unified Source Model, BL-Lacs, FR-I’s, … are all Accreting Super-Massive Black Holes Tom Weiler, Vanderbilt & CERN

  45. Nearest are Cen-A (3.4 Mpc) in South and M87 (16 Mpc) in North Ergo, may be the best candidate Xgal neutrino sources The n-mixing thm predicts a nearly equal flux for each flavor “j”, normalized to the g-ray flux as (factor 2 from scaling energy bin) The resulting n flux on Earth from Cen-A during a bursting phase (~ yr, Narrabri 4.5s, 1970s) is  Prediction: Tom Weiler, Vanderbilt & CERN

  46. And for M87: • From HEGRA, 4.1s, 98-99 • Consistent with Cen-A and 1/r2 • ~ 2 events/yr in IceCube, similar to atmospheric background The diffuse flux on Earth then follows: leadingto: between bursts. Tom Weiler, Vanderbilt & CERN

  47. Auger neutrons form Cen-A Since ctn = 0.9 Mpc E20, Neutron survival probability from Cen-A = e –3.8/E20 = 2% at 1020 eV = 15% at 2 1020 eV = 1/e at 3.8 1020 eV Maybe 2 evts/yr at Auger, more at EUSO, with Glennys’ flux (Farrar-Piran) Anchordoqui, Goldberg, TJW; hep-ph/01 Tom Weiler, Vanderbilt & CERN

  48. m3 m3 m2 m2 m1 m1 nm ne nt Or maybe … It looks like this Log m2 Tom Weiler, Vanderbilt & CERN

  49. Dirac neutrino vs Majorana neutrino • Majorana Dirac Lorentz Boost, E, B C P T C P T So is a Dirac just two Majoranas? Yes, iff the two Majoranas are mass-degenerate and have opposite CP parity Tom Weiler, Vanderbilt & CERN

  50. Pseudo-Dirac Mass Spectrum Beacom, Bell, Hooper, Learned, Pakvasa, TJW Tom Weiler, Vanderbilt & CERN

More Related