1 / 26

Neutrino Physics

Neutrino Physics. José Bernabéu IFIC-University of Valencia December 2007. Neutrino Physics. History and Interest First evidence of neutrino masses Origin of masses? - Experiment - Beyond Standard Model Dimension 5: Majorana ’s Grand Unification Scale: See-saw Leptogenesis

ima
Download Presentation

Neutrino Physics

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Neutrino Physics José Bernabéu IFIC-University of Valencia December 2007

  2. Neutrino Physics • History and Interest • First evidence of neutrino masses • Origin of masses? - Experiment - Beyond Standard Model • Dimension 5: Majorana ’s • Grand Unification Scale: See-saw • Leptogenesis • CP-violation  Future experiments • Neutrino oscillations & Underground Physics

  3. The Birth of the Neutrino

  4. History: Up’s & Down’s 1930  Pauli, 1933  Fermi 1956  Cowan & Reines 1957  Two-component  theory: Weyl  Argument in favour of vanishing m Only L in weak interactions Goldhaber experiment 1958  (V-A) theory  CHIRAL Fields enter FOR ALL Fermions  Nothing special for ’s No reason why m =0 BUT: eR, qR needed QED, QCD 1967  Standard Model “choice”: no R  m=0 1998  m  0 experimentally…  Dirac Mass  0

  5. Neutrino Experiments

  6. Neutrino flavour oscillations What is known, what is unknown ? Absolute neutrino masses ? 3 H beta decay • Form of the mass spectrum • Matter effect in neutrino propagation Majorana neutrinos ?  0: masses and phases

  7. Origin of masses Why are Neutrino Masses so small? even for a smooth LOG – scale…

  8. The Pontecorvo MNS Matrix  For Flavour oscillations U: 3 mixings, 1 phase • Atmospheric K2K MINOS, CNGS Appearence e! Reactor Disappearence Matter in Atmospheric • Solar KAMLAND

  9. Neutrino oscillations After atmospheric and solar discoveries and accelerator and reactor measurements → θ13 , δ CP violation accessible in appearance experiments Appearance probability: |Ue3| gives the strength of P(ne→νμ) δ acts as a phase shift

  10. Beta/EC CERN Beam  ? Two methods: • Neutrino vs. Antineutrino - Energy Dependence

  11. LSC: Laboratorio Subterráneo de Canfranc

More Related