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Oscillation formalism

Oscillation formalism. Neutrino mixing Oscillations of 2 flavors Experimental sensitivities Oscillations in 3 flavors Discovery of oscillations: atmospheric neutrinos in Super-Kamiokande. Quark mixing in Standard Model. u c t d s b. States partcipating in strong

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Oscillation formalism

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  1. Oscillation formalism • Neutrino mixing • Oscillations of 2 flavors • Experimental sensitivities • Oscillations in 3 flavors • Discovery of oscillations: atmospheric neutrinos in Super-Kamiokande

  2. Quark mixing in Standard Model u c t d s b States partcipating in strong interactions with well defined masses (mass matrix eigenstates): u c t d` s` b` States participating in weak interactions: Quark mixing: „From neutrinos to cosmic sources”, DK & ER

  3. Neutrino mixing NOT in Standard Model IF neutrinos are massive: States with well defined masses (mass matrix eigenstates): States participating in weak interactions: Lepton mixing:

  4. Neutrino oscillation – 2 flavors mixing angle: mass states: ϑ are defined as different proportions ofν1 ,ν2 states ν1 ,ν2 states have different masses different velocities changes during propagation, hence The ratio

  5. Oscillation probability – 2 flavors A state of mass mk, energy and momentum Ek,pkpropagates: with phase: Let’s assume an initial state:

  6. Oscillation probability – 2 flavors During propagation the contribution of ν1,ν2 components changes: A probability that after t,x the state α is still in its initial α state: Finally:

  7. Oscillation probability – 2 flavors Probability of transition from a state α to a state β: oscillation parameters m-mass (in eV) ϑ - mixing angle experimental conditions: Eν – neutrino energy (in GeV) L- distance from a neutrino source to detector (km) Oscillation length:

  8. Appearance and disappearance experiments In an appearance experiment one searches for neutrinos νβ in an initial beam of να: In a disappearance experiment one counts how many of the initial neutrinos ναare left after passing a distance L: Note: Neutrino oscillate only if masses are non-zero and not the same

  9. Sensitivity to oscillations

  10. Graphic illustration ofneutrino oscillations For max mixing ϑ=π/4 and at a distance L=Losc/2 all the initial flavor νa are transformed to another flavor νb

  11. Transitions between 3 mass states With 3 generations there are 3 Δm2’s but only two are independent.

  12. Mixing of 3 flavors For 3 flavors we need 3x3 matrix. In quark case the corresponding matrix is called CKM (Cabibo-Kobayashi-Maskava). For neutrinos MNS (Maki-Nakagava-Sakata)

  13. Mixing of 3 flavors (part 2) The 3x3 matrix has 4 independent real parameters: where: 4 independent parameters: Current experiments are not sensitive to φ. It’s assumedφ=0

  14. Mixing of 3 flavors (part 3) The mixing matrix can be written: φ=0 rotation by: rotation by: rotation by: „From neutrinos to cosmic sources”, D.Kiełczewska, E.Rondio

  15. Oscillation Probability – 3 flavors (part 1) Per analogy with 2 flavor case the amplitude for the neutrino oscillation:

  16. How do Neutrinos Oscillate? Amplitude Amplitude

  17. Oscillation Probability – 3 flavors In a general case, with at least one non-zero complex phase: Note here: if α=β then the imaginary components disappear CP phase cannot be measured in disappearance experiments

  18. Oscillation Probability – 3 flavors (φ=0) a12 a13 a23

  19. Oscillation Probability – 3 flavors (φ=0) Let’s assume: Then we have 2 types of experiments: Case A – „atmospheric” - small L/E: Case B – „solar” - large L/E

  20. Oscillation probability – 3 flavors (φ=0) ∆m >>δm Case A – „atmospheric” - small L/E: Note: for ϑ13=0 all formulas are the same as for 2 flavors Case B – „solar” - large L/E

  21. More exact formula: one gets: By expanding in: + neutrinos - antineutrinos solar term CP violation L – baseline; We will introduce later: matter effects  sensitivity to mass hierarchy If LA<<1: The above formula is necessary for future, more exact studies

  22. Let’s try to understand atmospheric neutrino puzzle

  23. Neutrino events in Super-K All have to be separated from „cosmic” muons (3Hz) Contained events: Fully contained FC Partially contained PC Upward through-goingμ μ μ Upward stoppingμ μ all assumed to beμ e/μidentification interactions in rocks below the detector • different energy scale • different analysis technique • different systematics

  24. Neutrino energy spectra Fully contained FC Partially contained PC μ e/μidentification all assumed to be μ Upμ thru Upμ stop Interactions in rocks

  25. Super-Kamiokande results (contained) Sub-GeV(Fully Contained) Multi-GeV Evis < 1.33 GeV, Pe > 100 MeV, Pμ > 200 MeV Fully Contained (Evis > 1.33 GeV) Data MC 1ring e-like 772 707.8 μ-like 664 968.2 Data MC 1-ring e-like 32663081.0 μ-like 3181 4703.9 Partially Contained (assigned as m-like) 913 1230.0 We take ratios to cancel out errors on absolute neutrino fluxes: Too few muon neutrinos observed!

  26. Super-Kamiokande I results - upward going muons Up through-going μ, (1678days) Data: 1.7 +- 0.04 +- 0.02 (x10-13cm-2s-1sr-1) MC: 1.97+-0.44 Up stopping μ, (1657days) Data: 0.41+-0.02+-0.02(x10-13cm-2s-1sr-1) MC:0.73+-0.16 Again one observes a muon deficit

  27. Super-Kamiokande evidence for neutrino oscillations

  28. Interpretation of the zenith angle distributions Let’s try to find interpretation of the deficit of νμ after passing the Earth ...... Looks like νμdisappearance... What happens to muon neutrinos? Let’s suppose an oscillation: but what is We see that ne angular distribution is as expected

  29. Oscillations of muon neutrinos Looks like νμ oscillates:.. Remember that we identify neutrinos by the corresponding charged lepton which they produce: But look at the masses: μ 106 MeV τ 1777 MeV Does neutrino have enough energy to produce τ ?

  30. ντ cross sections Total CC cross sections for: compared with νμ masses:μ 106 MeV τ 1777 MeV

  31. We don’t see the neutrinosafter oscillations! • The cross section for CC interaction (with τ ) too small • NC interactions possible but • then we cannot tell • the neutrino flavor!

  32. Rough estimate of Eν– neutrino energy (inGeV) L- distance (km) Oscillation length: Max probability of oscillation for L=Losc/2 Find corresponding Down, L=15 km Up, L=12000 km For Eν=1 GeV For Eν=10 GeV For Eν=100 GeV The trouble is – we don’t know precisely Eν

  33. Sensitivity of angular distribution to neutrino oscillations Expected angular distributions for oscillations with various mass parameters for the neutrino energy distribution of multi-GeV sample. No oscillations 10-2 10-3 Δm2 = 10-4 10-1 Sensitivity from ~10-4 to 10-1 eV2 Up-going Down-going

  34. Zenith angle distributions e-like 1 ring μ-like 1 ring μ-like multi- ring upward goingμ Sub-GeV Multi-GeV Red: MC expectations Black points: Data Green: oscillations Missing are the muon neutrinos passing through the Earth! down up

  35. Super-K up-down asymmetry expected- no oscil Data with -oscillations

  36. Rough estimate of the mixing angle Probability of νμdisappearance... For large distancesL oscillations happen for a variety of Eν, so that one should take: Then: (at some angles we see half of neutrinos disappearing) i.e. maximal mixing

  37. Definition of 2 for oscillation analysis A fit is performed i.e. a minimum of χ2 is found. The corresponding arethe best fit oscillation parameters

  38. Results of combined fit c2vs Dm2 flat between 0.0019 and 0.0025

  39. Contours for different subsamples Sub-GeV 1-ring e-like 3353 Sub-GeV 1-ring μ-like 3227 Multi-GeV 1-ring e-like 746 Multi-GeV 1-ring μ-like 651 PC μ-like 647 Multi-ring 647Upward muons 2259 ------All 11530

  40. Oscillation parameters from different experiments (atmospheric)

  41. L/E analysis of the atmospheric neutrino data from Super-Kamiokande

  42. From neutrinos to cosmic sources, DK&ER Hypotheses other than oscillation Neutrino oscillation : Neutrino decay: Neutrino decoherence : Idea: use events with the best resolution in L/E

  43. From neutrinos to cosmic sources, DK&ER Reconstruction of Eν and L Neutrino energy Neutrino direction Eobserved  Eν Zenith angle  Flight length Neutrino energy is reconstructed from observed energy using relations based on MC simulation Neutrino flight length is estimated from zenith angle of particle direction

  44. From neutrinos to cosmic sources, DK&ER Neutrino path-length L vs angle Very bad Close to the horizon

  45. From neutrinos to cosmic sources, DK&ER Survival probability divide DATA/MC Null oscillation MC Best-fit expectation 1489.2 days FC+PC A dip just where oscil. min expected

  46. From neutrinos to cosmic sources, DK&ER Test for neutrino decay & neutrino decoherence Oscillation Decay Decoherence Alternative hypotheses excluded.

  47. From neutrinos to cosmic sources, DK&ER Oscillation analysis – fitting L/E distribution

  48. Atmospheric neutrino experiments The largest statistics of atmospheric neutrino events were collected in Super-Kamiokande. The results showed: a deficit of muon neutrinos passing long distances through the Earth. first evidence of neutrino oscillatons Atmospheric neutrinos were also measured in MACRO and SOUDAN detectors. The results were consistent with neutrino oscillations.

  49. From neutrinos to cosmic sources, DK&ER Summary: evidence of oscillations in atmospheric neutrinos • Missing Effect observed in different Super-K event samples and also by other experiments Stat. significance above 10 sigmas • Angular distributions probability of disappearance depends on its path-length and energy in a way consistent with oscillation • survival dependnce on L/E only oscillations can produce a dip • Oscillation parameters from comparison between data and MC simulations:

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