1 / 20

Probing the Broken  -  Symmetry with Neutrino Telescopes

Probing the Broken  -  Symmetry with Neutrino Telescopes. Zhi-zhong Xing (IHEP, Beijing). NOW 2006 Conca Specchiulla, September 9 - 16, 2006. Z.Z.X. hep-ph/0605219 Phys. Rev. D 74 (2006) 013009. Outline. 1. UHE Neutrinos: the Oscillating Messenger.

zwi
Download Presentation

Probing the Broken  -  Symmetry with Neutrino Telescopes

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. Probing the Broken-Symmetry with Neutrino Telescopes Zhi-zhong Xing (IHEP, Beijing) NOW 2006 Conca Specchiulla, September 9 - 16, 2006 Z.Z.X. hep-ph/0605219Phys. Rev. D 74 (2006) 013009

  2. Outline 1. UHE Neutrinos: the Oscillating Messenger 2. -Telescope as a Probe of - Symmetry 3. Further Discussion and Concluding Remarks

  3. UHE Neutrinos

  4. CMB Light absorbed (1e:1:1) Neutrino (1e:2) Proton scattered by magnetic field neutrino photon proton PeV EeV TeV ZeV Log E (GeV) 1 2 3 4 5 6 7 8 9 10 11 12 13 High-energy Cosmic Messengers straight-line propagation, unabsorbed, but difficult to detect “somebody really really wise” (Tom Weiler at Neutrino 2006) a sufficiently large neutrino detector ---neutrino telescopes

  5. ANTARES La-Seyne-sur-Mer, France BAIKAL Russia NEMO Catania, Italy NESTOR Pylos, Greece AMANDAandIceCube South Pole, Antarctica Optical Cherencov -Telescopes

  6. Halzen, astro-ph/0602132 17m Learned & Pakvasa 95 How to identify Neutrino Flavors?

  7. Point One Point Two The Starting Point of View First of all, discover something Next, measure it precisely Our concern: Initial flavor composition of UHE neutrino fluxes and their oscillations

  8. Incomplete List of Relevant Works ■Learned & Pakvasa, APP 3, 267 (1995) ★ Athar et al, PRD 62, 103007 (2000) ★ Bento et al, PLB 476, 205 (2000) ★ Gounaris & Moultaka, hep-ph/0212110 ★Barenboim & Quigg, PRD 67, 073024 (2003) ★ Beacom et al, PRD 68, 093005 (2003) ★ Keraenen et al, PLB 574, 162 (2003) ★ Beacom et al, PRD 69, 017303 (2004) ★ Serpico & Kachelriess, PRL 94, 211102 (2005) ★ Bhattacharjee & Gupta, hep-ph/0501191 ★ Serpico, PRD 73, 047301 (2006) ●Xing, PRD 74, 013009 (2006) ●Xing & Zhou, PRD 74, 013010 (2006) ★ Winter, PRD 74, 033015 (2006) ■Fogli et al, hep-ph/0608321 ★ Majumdar & Ghosal, hep-ph/0608334

  9. The transition probability: The expected sources (AGNs etc) at typical distances: ~100 Mpc For , the oscillation length in vacuum So after many oscillations, the averaged transition probability of UHE neutrinos is atmosphere UHE Neutrino Oscillations

  10. - symmetry at 99% C.L. (Strumia & Vissani 06) Data and Approximation A global analysis of current neutrino oscillation data yields

  11. Broken - Symmetry

  12. High-energy pp collisions:  charged poins  muon and electron neutrinos High-energy p collisions: There is no production of electron antineutrino, because the produced neutrons can escape the source before decaying (M. Ahlers et al, 05) In either case, the sum of neutrinos and antineutrinos Conventional UHE Neutrino Source

  13. At the detectors of neutrino telescopes: Two small parameters to measure tiny-symmetry breaking: Effect of -Symmetry Breaking

  14. The allowed range of: ZZX: hep-ph/0605219 Correction to the Naïve Ratio 1:1:1 The boundappears when two small - symmetry breaking parameters turn to take their maximal (upper limit) values

  15. Yes, if the following relation is by accident satisfied: The working observables: Signals at Neutrino Telescopes Can =0 nontrivially hold? A signal of   0is in general expected, however. It makes senseto consider the complementarity between neutrino telescopes and terrestrial neutrino oscillation experiments, in order to finally pin down the parameters of neutrino mixing and CP violation. (Winter, hep-ph/0604191)

  16. A novel possibility to detect the UHE electron anti-neutrino flux from distant astrophysical sources (S.L. Glashow 60): A neutrino telescope may measure:(a)the GR-mediated electron anti-neutrino events;(b)the muon neutrino  muon anti-neutrino charged-current interaction events in the vicinity, to extract Comment 1: it is possible to probe the-symmetry breaking; Comment 2: it is likely to probe the solar neutrino mixing angle. Glashow Resonance

  17. Concluding Remarks

  18. The initial flavor composition of UHE neutrino fluxes should be determined experimentally • Neutrino telescopes can do this, at least in principle Do Flavor Physics with -Telescopes • The astrophysical sources of UHE neutrinos: puzzles • Do ultra-long baseline & ultra-high energy neutrino oscillation experiments with ultra-large-telescopes? Z.Z.X. & S.Zhou: Phys. Rev. D 74 (2006) 013010 • Given a well-understood source, a neutrino telescope can help determine the neutrino mixing parameters • There is a lot of important complementarity between terrestrial neutrino experiments & neutrino telescopes

  19. The Mediterranean Sea The South Pole Search for ’s at Wonderful Places

  20. Source Detector Unless there is an exact - flavor symmetry! Last but not Least Thanks a lot

More Related