20061019 1732 oberauer hql06

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Published on November 15, 2007

Author: Barbara

Source: authorstream.com

Astrophysical Neutrinos:  Astrophysical Neutrinos Neutrinos as probes HQL, Munich, October 16th-20th, 2006 L. Oberauer, TU Munich Slide2:  Energy Spectra of Astrophysical Neutrinos thermal sources Non-thermal sources Slide3:  Pion production and subsequent decays (incl. muon) p -> m + nm m -> e + nm + ne Oscillations and Atmospheric Neutrinos Slide4:  Atmospheric Neutrinos and SuperKamiokande Charged current reactions nm + N -> m + N` and ne + N -> e + N` 50 kt Water Cherenkov Detector Slide5:  νμ νe Electron events Muon events Up going Up going Neutrinos m e No-oscillation Oscillation Slide6:  Result atmospheric Neutrino-Oscillations Best fit: m2atm = 2.5×10-3 eV2 sin22θatm = 1.0 Confirmed by MACRO (Gran Sasso) Soudan (USA) K2K accelerator long baseline (250 km) experiment MINOS (USA) acc. exp. in 2006 Slide7:  Oscillations and Solar Neutrinos Sudbury Neutrino Observatory SNO:  Sudbury Neutrino Observatory SNO charged current interaction (cc) ne + D -> p + p + e neutral current interaction (nc) nx + D -> nx + p + n elastic Neutrino-Electron scattering (cc + nc) nx + e -> nx + e 1kt Cherenkov Detector with heavy water SNO Result :  SNO Result Flavour transition discovered: 7 sigma ! Reasonable agreement with solar model Neutrinos from the Sun (ne) transform into nm or nt ! Solar Neutrino Oscillation:  Solar Neutrino Oscillation Determination of Q12 ~ 340 ne nm,t Dm2 ~ 8 x 10-5 eV2 Confirmation by reactor experiment KamLAND The solar matter effect – evidence by GALLEX/GNO:  The solar matter effect – evidence by GALLEX/GNO GALLEX/GNO SNO Evidence for matter effect inside the Sun m2 > m1 Why are neutrino masses so small? GUT Leptogenesis Survival probability electron neutrino pp- 7Be 8B Future of Solar Neutrino Spectroscopy: low energies :  Future of Solar Neutrino Spectroscopy: low energies Monoenergetic 7Be CNO, pep Why? Accurate Measurement of thermo nuclear fusion processes: 7Be ~ 10% => pp ~ 1% ! CNO important for star development The MSW Effect and new Physics ?:  The MSW Effect and new Physics ? Friedland, Lunardini, Peña-Garay, hep-ph/0402266 The MSW effect as filter Q13 sterile Neutrinos? magnetic Neutrino moment? new interactions ? Water filling started in August 2006:  Water filling started in August 2006 BOREXINO sees neutrinos from CERN (August 2006) !:  BOREXINO sees neutrinos from CERN (August 2006) ! Slide17:  First neutrino events in BOREXINO Time of flight (CERN to LNGS) ~ 2.4 ms equivalent to ~ 730 km distance Future Neutrino Observatories:  Future Neutrino Observatories Unsegmented 50 kt liquid scintillator LENA HyperKamiokande (1 Mt Water Cherenkov) …Liquid Argon ~100 kt TPC LAGUNA:  LAGUNA Large Aparatus for Grand Unification and Neutrino Astronomy European initiative (France, Germany, Italy, Switzerland, UK, Poland, Finland) Aim: Design studies for all 3 kinds of detectors (water Ch, scintillator, liquid argon) until ~ 2010 Physics goals of future Neutrino Observatories:  Physics goals of future Neutrino Observatories Gravitational collapse Star formation rate in the early universe Thermonuclear fusion reactions Baryon number violation (Proton decay) Leptonic CP – violation Geophysics Indirect search for Dark Matter Active Galactic Nuclei – UHE Neutrinos One example for LENA: Detection of the Diffuse Supernova Neutrino Background (DSNB) ?:  One example for LENA: Detection of the Diffuse Supernova Neutrino Background (DSNB) ? up to now only limits flux and spectral shape depend on Star formation rate Gravitational collapse model Extremely Large Observatories:  Extremely Large Observatories Km3 Cherenkov detector in the mediterranian sea Km3 Cherenkov detector at the South Pole (Ice Cube) Slide23:  Amanda Frejus Eν  E-3.8 A change in the slope would indicate a non-atmospheric component Atmospheric neutrino Waxmann-Bahcall limit: Model-independent upper bound = 2 = 00-03 combined Limits from Amanda Ice-Cube ~ 3 10-9 Conclusions:  Conclusions Neutrino physics very successfull in the last decade Neutrino masses and mixing established Physics beyond the standard model New window to astrophysical observations

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