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Lecture 3 – neutrino oscillations and hadrons

Lecture 3 – neutrino oscillations and hadrons. Review of leptons Neutrino oscillations Introduction to hadrons. The lepton family. Spin 1/2. 6 leptons + antileptons. Divided into 3 families/flavours/multipletes: electron,muon tau. Lepton interactions. e -. m -. m -. e -. e -. W -.

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Lecture 3 – neutrino oscillations and hadrons

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  1. FK7003 Lecture 3 – neutrino oscillations and hadrons • Review of leptons • Neutrino oscillations • Introduction to hadrons

  2. FK7003 The lepton family Spin 1/2 6 leptons + antileptons. Divided into 3 families/flavours/multipletes: electron,muon tau

  3. Lepton interactions e- m- m- e- e- W- g nm m+ Charged leptons interact via the em and weak forces. Neutrinos only interact via the weak force. Lepton number is always conserved at a vertex and in the whole process. As for all forces: Charge conservation and energy-momentum conservation for incoming and outgoing particles. Charge is conserved at a vertex though energy can appear to be violated when dealing with ”internal lines” (lecture 1). FK7003

  4. FK7003 Neutrino masses

  5. FK7003 Neutrino oscillations m+ p+ Conserves Lm nm Conserves Lt nt t- Whole process violates: Lm, Lt

  6. FK7003 Neutrino oscillation formalism

  7. Real(ni) Real(ni) Real(na) L nbprobability FK7003 naprob. naprob.

  8. FK7003 109 106 103 106 1 103 Neutrino Interactions in Matter l I(x) I0 n Neutrino interaction lengthi In water/km 0 x  interaction E  (TeV) Probability of interaction ~ 10-5/ km water at 100 TeV energy 100 billion neutrinos pass through your thumbnail each second but only 1-2 will interact in your body during your lifetime.

  9. FK7003 Neutrinos arriving at Earth – not for the exam Relevant for this lecture relics from Big Bang nuclear reactions in Sun explosions of supernova Flux/energy (cm-2s-1MeV-1) natural radioactive decay in Earth nuclear reactors remnants of supernova interactions of cosmic rays in atmosphere Active Galactic Nuclei Neutrino energy (eV)

  10. FK7003 Atmospheric neutrinos and Super Kamiokande Boat

  11. FK7003 Super-K: nm oscillations From above 15 km Super-K no oscillations P(nm nm) (Data/Prediction for oscillations) oscillations Earth From below 13000 km

  12. FK7003 Atmospheric neutrino results E=1 GeV

  13. FK7003 Neutrinos arriving at Earth – not for the exam Relevant for this lecture relics from Big Bang nuclear reactions in Sun explosions of supernova Flux/energy (cm-2s-1MeV-1) natural radioactive decay in Earth nuclear reactors remnants of supernova interactions of cosmic rays in atmosphere Active Galactic Nuclei Neutrino energy (eV)

  14. FK7003 Neutrinos in the sun – not for the exam • Fusion process leading toaa • knemeasured flux on earth can be predicted Solar neutrino energies

  15. Solar neutrino problem FK7003

  16. FK7003 SNO

  17. FK7003 Results

  18. FK7003 Generalise for 3 neutrinos

  19. Mass2 (eV2) Flavour composition of mass state. 0.003 0.0001 FK7003

  20. FK7003 Question

  21. FK7003 Question

  22. FK7003 Question

  23. FK7003 Summary of neutrino oscillations • Neutrinos produced in the weak force are flavour eigenstates but not mass eigenstates. • Neutrino oscillations between flavours occur as a consequence of non-zero mixing angles and a non-zero difference between the mass states • Experiments on atmospheric and solar neutrinos demonstrate neutrino oscillations.

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