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Exploring the Status and Future of Neutrino Physics: Insights and Open Questions

In this presentation by Björn Wonsak, we delve into neutrino physics, motivated by unanswered questions in our understanding of the universe, such as those related to the Standard Model, matter-antimatter asymmetry, and astrophysical phenomena. We explore the phenomenon of neutrino oscillations, their implications for particle physics, and the methods used to study rare effects through interferometry and coherent sources. We also address open questions for future experiments, including CP violation and mass hierarchy among neutrinos, and outline upcoming initiatives in neutrino research that promise to illuminate these mysteries.

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Exploring the Status and Future of Neutrino Physics: Insights and Open Questions

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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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