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LAGUNA

LAGUNA. L arge A pparatus for G rand U nification and N eutrino A strophysics. Launch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM. Why ?. Neutrinos oscillations => New Particle Physics Main line besides future accelerator experiments

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LAGUNA

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  1. LAGUNA Large Apparatus for Grand Unification and Neutrino Astrophysics Launch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM

  2. Why ? Neutrinos oscillations => New Particle Physics • Main line besides future accelerator experiments • Baryon number violation ? => Nucleon decay(Search for Proton Decay) • Baryon asymmetry  Leptogenesis ? Q13, CP violation in leptonic sector ? (Long Baseline Neutrino Experiments)

  3. Astrophysics New Neutrino Observatories wanted Neutrinos as probes • Study of gravitational collapse(Supernova Neutrinos) • Study of star formation in the early universe (Diffuse Supernovae Neutrinos Background) • Precision study of thermonuclear fusion processes(Solar Neutrinos) • Test of geophysical models(Geoneutrinos)

  4. LENA • Low Energy Neutrino Astronomy • Diffuse Supernovae Neutrino Background • Supernova Neutrinos • Solar Neutrinos • Geoneutrinos • Proton Decay

  5. LENA: Diffuse SN Background ne + p -> e+ + n ~25% of events are due to v’soriginating from SN @ z>1! Rates depend on: supernova model, star formation rate, neutrino mass hierarchy Range 20 to 220 / 10 years “most probable” value ~ 100 Information on Supernova models & Star Formation rate (z~2) M. Wurm et al., Phys. Rev D 75 (2007) 023007

  6. LENA: Diffuse SN Background • optical measurements will determine the SNR with high accuracy • with this input, the spectral slope of the DSN can be used to distinguish between different SN explosion scenarios comparison of count ratesin the energy bins10MeV < EB1 < 14MeV15MeV < EB2 < 25MeV

  7. LENA: Supernova Neutrinos Assumption: Supernova II with 8 solar masses at 10 kpc distance ne flux and spectrum ne flux and spectrum

  8. LENA: Supernova Neutrinos Total neutrino flux Total energy spectrum

  9. LENA: Supernova Neutrinos Depending on threshold: p, nu - scattering dominated by nmandnt n + p -> n + p Threshold ~ 50 pe (photoelectrons)

  10. LENA: Solar Neutrinos LENA Fiducial Volume for solar n: 18 x 103 m3 • High statistic ( ~ 5.4 x 103 / day ) 7Be n + e ->n + e • test of small flux fluctuations in time • CNO and pep – neutrinos ( ~ 3 x 102 / day ) • solar neutrino luminosity • contribution of CNO cycle to solar energy release • Charged current ne (13C,13N) e- reaction ( ~ 103 / year ) • spectroscopy of 8B-n at energies below 5 MeV • (A. Ianni et al., hep-ph/0506171)

  11. LENA: Solar Neutrinos Non standard Interactions ? (e.g. flavor changing neutral currents) Standard MSW scenario 7Be pep CNO 8B Friedland, Lunardini, Peña-Garay, hep-ph/0402266

  12. CNO and the age of Globular Clusters • 14N(p,g)15O new value? (new result from LUNA) • Prediction CNO-n altered by factor ~2 • Age of Globular Clusters increased by factor 0.7 bis 1 Gy ! • Measurement of CNO -n : determination of metallicity in the centre of the Sun

  13. LENA: Solar Neutrinos Electron recoil spectrum Requirements: low background levels in U, Th, 210Pb at least ~4000 m.w.e. shielding

  14. LENA: Geo Neutrinos • Detection via inverse beta decay • measurement of radiogenic contribution to terrestrial heat (~ 40 TW) • test of the Bulk Silicate Earth model • test of unorthodox models of Earth‘s core (is there a breeder reactor ?)

  15. Rate of Geo-neutrinos in LENA LENA @ Pyhäsalmi: ~ 1.5 x 103 events / year Scaling KamLAND result to LENA: between 3 x 102 and 3 x 103 events / year Positron spectrum (arb. units) Reactor BG Uranium Uranium + Thorium

  16. Proton Decay in Supersymmetry SU(5) • GUT scale: • Preferred decay modes: • = (0.3 – 3) 1034y (S.Raby et al, 2002) • < 1035y (Babu, Pati, Wilzcek, 1998)

  17. Proton Decay(non SUSY) (P. Nath 2006) Limits from SuperKamiokande:

  18. LENA: Proton Decay

  19. LENA: Proton Decay

  20. LENA: Separartion e- m-like events ?

  21. Conclusions • LAGUNA – Design study for a large future European observatory (Water, Argon, Scintillator) • design study until ~ 2011 • on APpec road map for Launch after design study completed • LENA – Physics Potential in Low Energy Neutrino Astronomy and Proton Decay • Proton Decay: T. Marrodan-Undagoitia et al., Phys. Rev. D 72 (2005) 075014 • Geo-Nus: K.. Hochmuth et al., Astropart. Phys. 27 (2007) 21 • DSNB: M. Wurm et al., Phys. Rev. D 75 (2007) 023007

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