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Exploring Massive Neutrinos: Theory and Observations

Dive into the realm of massive neutrinos, from theory to observations in various sources like reactors, accelerators, and cosmic backgrounds. Learn about neutrino properties and their potential as dark matter candidates.

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Exploring Massive Neutrinos: Theory and Observations

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  1. Neutrinos Theory ~ Carlos Pena Garay IAS, Princeton Benasque

  2. References Neutrino Unbound http://www.nu.to.infn.it/

  3. Massive Neutrinos : Dirac n(p,h) n(p,-h) CPT Boost, if m ≠ 0 Boost, if m ≠ 0 n(p,-h) n(p,h) CPT

  4. Standard Model + right handed

  5. Standard Model + right handed

  6. Parameters : Dirac Exercise

  7. Wave packets : Neutrino osc. Relativistic neutrinos : Same result

  8. Size of the wave packet Coherent neutrino emission in plasma : Interrupted by e.m interactions of the source particles (pressure broadening) Reactor : e.m. interactions of produced e- Accelerator : time scale of weak interactions

  9. Matter effects Only the difference of potential is relevant Net effect :

  10. Some Neutrino Sources

  11. Solar

  12. Atmospheric

  13. Reactor : …,Chooz/Palo Verde,…

  14. Reactor : …,KamLAND

  15. Accelerator : K2K

  16. LMC 8GeV Booster magnetic horn decay pipe 450 m dirt detector absorber 25 or 50 m and target LSND, Miniboone Proton beam producing

  17. The Neutrino Matrix :SM + n mass 3 s ranges: ALL oscillation neutrino data BUT LSND

  18. The Neutrino Matrix : SM + n mass 1 s ranges: ALL oscillation neutrino data BUT LSND

  19. SM + n mass Neutrinos: Cosmological dark matter to be discovered If lowest mass is negligible, and normal hierarchy If highest mass is 1 eV

  20. Plan • I. Neutrinos as Dirac Particles • Making Neutrinos • Neutrinos as Majorana Particles

  21. Neutrino Sources Reactor Accelerator

  22. Cosmic Neutrino Background 56 cm-3 at 1.9K (0.17 meV) Possible mechanical effect : torque of order GF if target and neutrino background are polarized (Stodolsky effect) and net neutrino-antineutrino asymmetry Still far from observability, awaiting for future technology

  23. Photo (Compton) Plasmon decay Pair annihilation Bremsstrahlung Neutrinos from Thermal Plasma

  24. Solar (thermonuclear) Neutrinos Ga Cl SK, SNO

  25. Thermonuclear Neutrinos

  26. Geoneutrinos

  27. Sanduleak -69 202 Supernova 1987A23 February 1987 Tarantula Nebula Large Magellanic Cloud Distance 50 kpc (160.000 light years)

  28. Newborn Neutron Star Collapse (implosion) Explosion ~ 50 km Neutrino Cooling Proto-Neutron Star r  rnuc= 31014 g cm-3 T  30 MeV Stellar Collapse and Supernova Explosion

  29. Neutrino Signal of Supernova 1987A Kamiokande (Japan) Water Cherenkov detector Clock uncertainty 1 min Irvine-Michigan-Brookhaven (US) Water Cherenkov detector Clock uncertainty 50 ms Baksan Scintillator Telescope (Soviet Union) Clock uncertainty +2/-54 s Within clock uncertainties, signals are contemporaneous

  30. Limits on Supernova Relic Neutrinos Super-Kamiokande : Ando et al (2004)

  31. Atmospheric Neutrinos

  32. Undiscovered neutrino sources Neutrinos from the Sun    Neutrinos from the Earth  + 

  33. Sources above 10GeV GRBs? by Eli Waxman

  34. Sources above 10GeV 90% CL upper limits in 10-8 cm-2s-1 for E-2 spectrum from AMANDA II (2000-2002) :

  35. E-2.7 E-3.0

  36. Flavor ratio for far p sources

  37. Man-made Neutrino Sources : Reactors Goal : Measure q13

  38. conventional beams / superbeams • b-beams • neutrino factories Man-made Neutrino Sources : Accelerator

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