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Status and Future of n -physics

Status and Future of n -physics. What do I talk about?. Motivations Oscillations Status Open Questions Near Future Not so far Future Conclusions. Why are we doing ν -physics?. SM is very successful but it leaves a lot of questions open

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Status and Future of n -physics

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  1. Status and Future of n-physics Björn Wonsak

  2. What do I talk about? • Motivations • Oscillations • Status • Open Questions • Near Future • Not so far Future • Conclusions Björn Wonsak

  3. Why are we doing ν-physics? • SM is very successful • but it leaves a lot of questions open (e.g. astrophysical questions, like big bang, matter-antimatter asymmetry, supernovaes, etc.) we want to understand physics beyond the SM • There are two ways to do that: • High Energies bigger accelerators • Study rare, tiny effects more statistics, lower background Björn Wonsak

  4. Why are we doing ν-physics? • Tiny effect (mn/En)2~(eV/GeV)2=10–18 ! • Suitable methode: Interferometry • Needs coherent source • Needs Interference (i.e., large mixing angles) • Needs long baseline • All this is given us by nature: Neutrino Interferometry (Oscillations) is a unique tool to study physics at very high scales !!! Lowest order effect of physics at short distances !!! Björn Wonsak

  5. What are ν-oscillations? • Flavour eigenstates ne,m,tare not the mass eigenstates n1,2,3 neutrino mixing Pontecorvo-Maki-Nakagawa-Sakata (PMNS) Matrix: • This leads to oscillations between the ne,m,t like in the Kaon system • ν must have different masses (not all are massless) • Leptonflavour is not strictly conserved Already beyond the SM ! Björn Wonsak

  6. What are ν-oscillations? propagation determined bymass-eigenstates source createsflavor-eigenstates detector seesflavor-eigenstates v2 τ vτ v3 vμ W W μ p,n hadrons slightly different frequencies→ phase difference changes Mass eigenstates n2,n3with m2, m3 Flavor eigenstates nm, nt Björn Wonsak

  7. What are ν-oscillations? Probability to find vτ Distance x in Losz • Oscillation probability with experiment needs energy resolution experiment needs statistics sin2(2θ) Losz, Δm2 Björn Wonsak

  8. What are ν-oscillations? Zero for CP conservation Three flavour mixing: 3 mixing angles and 1 CP-violating phase If neutrinos are Majorana particles: 2 additional Majorana-Phases (CPV): α1, α2 Björn Wonsak

  9. Example for 3 flavour Oscillation probability ! L/E is crucial ! sin2(2q13) sin2(2q12) Dm213 Dm212 Björn Wonsak

  10. What do we know? • Atmospheric neutrinos Super-Kamiokande Atmosphärische nBeschleuniger n Björn Wonsak

  11. What do we know? • Solar neutrinos SNO KamLAND Reaktor-n Solar-n Mass effects in the sun dominate ! Björn Wonsak

  12. What are ν-oscillations? Three flavour mixing: 3 mixing angles and 1 CP-violating phase Very different Dm2 in different sectors Solar and atmospheric oscillations can be regarded as independent 2 flavor discription is sufficient If neutrinos are Majorana particles: 2 additional Majorana-Phases (CPV): α1, α2 Björn Wonsak

  13. What do we want to know? bb0n: claim by Klapdor-Kleingrothaus ! • Dirac or Majorana ? • Absolute mass scale ? • How small is θ13 ? • CP-violation ? • Mass hierarchy ? • Verify Ocsillations ? • LSND ? Sterile neutrinos ? CPT-violation ? direct measurement: Katrin aims for mn<0,2eV Diappearance energyspectra, nt apperance • can be adressed by oscillation experiments • need specialised experiments Björn Wonsak

  14. What comes next? NUMI MINOS 735km Minos started this year Magnetized steel/scintillator calorimeter • low E neutrinos (few GeV): nm disappearance experiment • 4 x1020 pot/year  2500 nm CC/year • compare Det1-Det2 response vs E  in 2-6 years sensitivity to Dm2atm • main goal: reduce the errors on Dm223 and sin22q23 as needed for sin22q13measurement Björn Wonsak

  15. NC/CC ratio measured contains four neutrino interactions Björn Wonsak

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  17. What comes next? nτ appearance experiment start end 2006 (search for q13) Emulsion CloudChamber (ECC) 1,8 kton mass En≈ 17 GeV Björn Wonsak

  18. Basic “cell” Target Trackers Pb/Em. target µ spectrometer 8 cm 8 m n Pb/Em. brick nt 1 mm Pb Emulsion Extract selected brick technic already used by Donut nt discovery anno 2000 Emulsion Analysis Vertex search Decay search e/γ ID, kinematics Electronic detectors select ν interacting brick µ ID, charge and p Björn Wonsak

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  20. What comes next? 100-200m 1 km 2 reaktors: 8.4GW Pth • Double Chooz 100-200 m 12.7 m3 12.7 m3 Search for θ13: Doppel-CHOOZ Reaktorneutrino experiment (France) first data taking beginning 2007 Double-Chooz sensitivity for (m2 = 2.0-2.5 10-3 eV2): sin2(213) < 0.025-0.03, 90% C.L. Björn Wonsak

  21. sin2(2q13) sin2(2q12) Dm213 Dm212 Double-Chooz Kamland Björn Wonsak

  22. What comes next to next? • monitor (beam direction and intensity) Same spectrum as SK, BG measurement n energy spectrum and intensity The first Super-Beam: off-axis T2K, from Tokai to SK start around 2009 Björn Wonsak

  23. 850km ne/ne appearance start about 2011 30kt liquid Scintillator detector NUMI beam with 6.5 x 1020 pot/yr With a new Proton Driver, 25 x 1020 pot/yr Superbeam! Bunch time information used n–physics comes back to surface 16mrad off-axis Björn Wonsak

  24. T2K NOvA with Neutrino superbeams Neutrino superbeams Björn Wonsak

  25. for maximal atmospheric mixing with Dm2≈2,5•10-3 eV2 Björn Wonsak

  26. What have we learned? • Smart way to reach high energy scales • Already physics beyond the SM • A lot of interesting open questions • First measurements were highly succesfull time for precision measurements • A new intertesting experiment every year fast growing knowledge Björn Wonsak

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