logging in or signing up 20061019 1732 oberauer hql06 Barbara Download Post to : URL : Related Presentations : Share Add to Flag Embed Email Send to Blogs and Networks Add to Channel Uploaded from authorPOINTLite Insert YouTube videos in PowerPont slides with aS Desktop Copy embed code: (To copy code, click on the text box) Embed: URL: Thumbnail: WordPress Embed Customize Embed The presentation is successfully added In Your Favorites. Views: 26 Category: Entertainment License: All Rights Reserved Like it (0) Dislike it (0) Added: November 15, 2007 This Presentation is Public Favorites: 0 Presentation Description No description available. Comments Posting comment... Premium member Presentation Transcript 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 sourcesSlide3: Pion production and subsequent decays (incl. muon) p -> m + nm m -> e + nm + ne Oscillations and Atmospheric NeutrinosSlide4: 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 OscillationSlide6: 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 2006Slide7: Oscillations and Solar NeutrinosSudbury 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 KamLANDThe 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 developmentThe 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 2006BOREXINO 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 distanceFuture 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 modelExtremely 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 10-9Conclusions: Conclusions Neutrino physics very successfull in the last decade Neutrino masses and mixing established Physics beyond the standard model New window to astrophysical observations You do not have the permission to view this presentation. In order to view it, please contact the author of the presentation.
20061019 1732 oberauer hql06 Barbara Download Post to : URL : Related Presentations : Share Add to Flag Embed Email Send to Blogs and Networks Add to Channel Uploaded from authorPOINTLite Insert YouTube videos in PowerPont slides with aS Desktop Copy embed code: (To copy code, click on the text box) Embed: URL: Thumbnail: WordPress Embed Customize Embed The presentation is successfully added In Your Favorites. Views: 26 Category: Entertainment License: All Rights Reserved Like it (0) Dislike it (0) Added: November 15, 2007 This Presentation is Public Favorites: 0 Presentation Description No description available. Comments Posting comment... Premium member Presentation Transcript 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 sourcesSlide3: Pion production and subsequent decays (incl. muon) p -> m + nm m -> e + nm + ne Oscillations and Atmospheric NeutrinosSlide4: 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 OscillationSlide6: 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 2006Slide7: Oscillations and Solar NeutrinosSudbury 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 KamLANDThe 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 developmentThe 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 2006BOREXINO 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 distanceFuture 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 modelExtremely 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 10-9Conclusions: Conclusions Neutrino physics very successfull in the last decade Neutrino masses and mixing established Physics beyond the standard model New window to astrophysical observations