\select@language {english}
\select@language {english}
\contentsline {section}{\numberline {1}Introduction}{1}{section.1}
\contentsline {subsection}{\numberline {1.1}Neutrino In a Nutshell}{1}{subsection.1.1}
\contentsline {subsection}{\numberline {1.2}Neutrino physics as part of the High Energy Physics Programme}{1}{subsection.1.2}
\contentsline {subsection}{\numberline {1.3}Implications and opportunities}{4}{subsection.1.3}
\contentsline {subsection}{\numberline {1.4}Precision measurements and sensitive searches}{6}{subsection.1.4}
\contentsline {subsection}{\numberline {1.5}What the study tried to achieve}{9}{subsection.1.5}
\contentsline {section}{\numberline {2}The Standard Neutrino Model}{11}{section.2}
\contentsline {subsection}{\numberline {2.1}Introduction}{11}{subsection.2.1}
\contentsline {subsection}{\numberline {2.2}Review of the present generation of experiments}{16}{subsection.2.2}
\contentsline {subsubsection}{\numberline {2.2.1}Solar and reactor neutrino experiments}{16}{subsubsection.2.2.1}
\contentsline {subsubsection}{\numberline {2.2.2}Atmospheric neutrino experiments}{20}{subsubsection.2.2.2}
\contentsline {subsubsection}{\numberline {2.2.3}Long-baseline neutrino-oscillation experiments}{23}{subsubsection.2.2.3}
\contentsline {subsubsection}{\numberline {2.2.4}$0\nu \beta \beta $ Experiments}{27}{subsubsection.2.2.4}
\contentsline {subsubsection}{\numberline {2.2.5}Recent progress in measurements of neutrino oscillations}{31}{subsubsection.2.2.5}
\contentsline {subsection}{\numberline {2.3}Completing the picture}{31}{subsection.2.3}
\contentsline {subsubsection}{\numberline {2.3.1}Bounds on $\theta _{13}$ from approved experiments}{32}{subsubsection.2.3.1}
\contentsline {subsection}{\numberline {2.4}Degeneracies and correlations}{34}{subsection.2.4}
\contentsline {subsubsection}{\numberline {2.4.1}Appearance channels: $\boldsymbol {\nu _e} \boldsymbol {\to } \boldsymbol {\nu _\mu }, \boldsymbol {\nu _\tau }$ and $\boldsymbol {\nu _\mu } \boldsymbol {\to } \boldsymbol {\nu _e}$ }{34}{subsubsection.2.4.1}
\contentsline {subsubsection}{\numberline {2.4.2}Disappearance channels: $\boldsymbol {\nu _\mu } \boldsymbol {\to } \boldsymbol {\nu _\mu }$ }{37}{subsubsection.2.4.2}
\contentsline {subsubsection}{\numberline {2.4.3}A matter of conventions}{39}{subsubsection.2.4.3}
\contentsline {subsubsection}{\numberline {2.4.4}Disappearance channels: $\boldsymbol {\nu _e} \boldsymbol {\to } \boldsymbol {\nu _e}$ }{40}{subsubsection.2.4.4}
\contentsline {section}{\numberline {3}Implications for new physics and cosmology}{40}{section.3}
\contentsline {subsection}{\numberline {3.1}The origin of small neutrino mass}{41}{subsection.3.1}
\contentsline {subsubsection}{\numberline {3.1.1}See-Saw mechanisms}{41}{subsubsection.3.1.1}
\contentsline {subsubsection}{\numberline {3.1.2}Supersymmetry and R-parity Violation}{43}{subsubsection.3.1.2}
\contentsline {subsubsection}{\numberline {3.1.3}Extra Dimensions}{48}{subsubsection.3.1.3}
\contentsline {paragraph}{\numberline {3.1.3.1}The effect of extra dimensions}{51}{paragraph.3.1.3.1}
\contentsline {subsubsection}{\numberline {3.1.4}String Theory}{52}{subsubsection.3.1.4}
\contentsline {subsubsection}{\numberline {3.1.5}TeV scale mechanisms for small neutrino masses}{55}{subsubsection.3.1.5}
\contentsline {subsection}{\numberline {3.2}Unification and Flavour}{60}{subsection.3.2}
\contentsline {subsubsection}{\numberline {3.2.1}Model survey}{60}{subsubsection.3.2.1}
\contentsline {subsubsection}{\numberline {3.2.2}Sum Rules}{69}{subsubsection.3.2.2}
\contentsline {subsubsection}{\numberline {3.2.3}Cabibbo Haze in Lepton Mixing}{74}{subsubsection.3.2.3}
\contentsline {subsection}{\numberline {3.3}Lepton-flavour violation}{80}{subsection.3.3}
\contentsline {subsection}{\numberline {3.4}Cosmology}{84}{subsection.3.4}
\contentsline {subsubsection}{\numberline {3.4.1}Neutrinos and Large Scale Structure}{84}{subsubsection.3.4.1}
\contentsline {paragraph}{\numberline {3.4.1.1}Impact of neutrinos on structure formation: theoretical predictions}{85}{paragraph.3.4.1.1}
\contentsline {paragraph}{\numberline {3.4.1.2}Current bounds}{88}{paragraph.3.4.1.2}
\contentsline {paragraph}{\numberline {3.4.1.3}Future prospects}{89}{paragraph.3.4.1.3}
\contentsline {subsubsection}{\numberline {3.4.2}Leptogenesis}{92}{subsubsection.3.4.2}
\contentsline {subsubsection}{\numberline {3.4.3}Neutrinos and Inflation}{96}{subsubsection.3.4.3}
\contentsline {section}{\numberline {4}Effects of New Physics beyond the Standard Neutrino Model}{99}{section.4}
\contentsline {subsection}{\numberline {4.1}Sterile neutrinos}{100}{subsection.4.1}
\contentsline {subsubsection}{\numberline {4.1.1}Theoretical issues}{100}{subsubsection.4.1.1}
\contentsline {subsubsection}{\numberline {4.1.2}Phenomenology of light sterile neutrinos}{101}{subsubsection.4.1.2}
\contentsline {subsubsection}{\numberline {4.1.3}Signatures of heavy sterile neutrinos}{102}{subsubsection.4.1.3}
\contentsline {subsubsection}{\numberline {4.1.4}Sterile neutrins and cosmology and astrophysics}{103}{subsubsection.4.1.4}
\contentsline {paragraph}{\numberline {4.1.4.1}Light, sterile neutrinos}{103}{paragraph.4.1.4.1}
\contentsline {paragraph}{\numberline {4.1.4.2}KeV sterile neutrinos}{103}{paragraph.4.1.4.2}
\contentsline {paragraph}{\numberline {4.1.4.3}MeV-GeV mass sterile neutrinos}{104}{paragraph.4.1.4.3}
\contentsline {subsubsection}{\numberline {4.1.5}The LSND challenge}{105}{subsubsection.4.1.5}
\contentsline {paragraph}{\numberline {4.1.5.1}Four-neutrino oscillations}{106}{paragraph.4.1.5.1}
\contentsline {paragraph}{\numberline {4.1.5.2}(2+2): ruled out by solar and atmospheric data}{107}{paragraph.4.1.5.2}
\contentsline {paragraph}{\numberline {4.1.5.3}(3+1): strongly dis-favoured by SBL data}{108}{paragraph.4.1.5.3}
\contentsline {paragraph}{\numberline {4.1.5.4}Global fit in four-neutrino schemes}{109}{paragraph.4.1.5.4}
\contentsline {paragraph}{\numberline {4.1.5.5}Five-neutrino oscillations}{110}{paragraph.4.1.5.5}
\contentsline {paragraph}{\numberline {4.1.5.6}Unconventional manifestations of leptonic-CP violation?}{111}{paragraph.4.1.5.6}
\contentsline {paragraph}{\numberline {4.1.5.7}More exotic explanations of LSND}{115}{paragraph.4.1.5.7}
\contentsline {subsection}{\numberline {4.2}Mass Varying Neutrinos}{116}{subsection.4.2}
\contentsline {subsection}{\numberline {4.3}CPT and Lorentz invariance violation}{119}{subsection.4.3}
\contentsline {subsubsection}{\numberline {4.3.1}Direct bounds on CPTV}{120}{subsubsection.4.3.1}
\contentsline {subsubsection}{\numberline {4.3.2}CPTV/LIV Effect on conversion probability}{121}{subsubsection.4.3.2}
\contentsline {subsubsection}{\numberline {4.3.3}Future Prospects}{122}{subsubsection.4.3.3}
\contentsline {subsection}{\numberline {4.4}Leptonic unitarity triangle and CP-violation}{122}{subsection.4.4}
\contentsline {subsubsection}{\numberline {4.4.1}Properties of the leptonic triangles}{123}{subsubsection.4.4.1}
\contentsline {subsubsection}{\numberline {4.4.2}Leptonic triangles and coherence of neutrino states }{124}{subsubsection.4.4.2}
\contentsline {subsubsection}{\numberline {4.4.3}The unitarity triangle and oscillation experiments}{126}{subsubsection.4.4.3}
\contentsline {subsubsection}{\numberline {4.4.4}Leptonic unitarity triangle and future experiments}{129}{subsubsection.4.4.4}
\contentsline {subsubsection}{\numberline {4.4.5}Beyond three neutrinos}{130}{subsubsection.4.4.5}
\contentsline {subsubsection}{\numberline {4.4.6}Constraints on unitarity}{131}{subsubsection.4.4.6}
\contentsline {subsection}{\numberline {4.5}Non-standard interactions}{134}{subsection.4.5}
\contentsline {subsubsection}{\numberline {4.5.1}Non-standard interactions in production and detection}{136}{subsubsection.4.5.1}
\contentsline {subsubsection}{\numberline {4.5.2}Non-standard interactions in propagation}{142}{subsubsection.4.5.2}
\contentsline {paragraph}{\numberline {4.5.2.1}Parameters and limits:}{142}{paragraph.4.5.2.1}
\contentsline {paragraph}{\numberline {4.5.2.2}Effects on neutrino propagation}{145}{paragraph.4.5.2.2}
\contentsline {subsubsection}{\numberline {4.5.3}Constraints from non-oscillation neutrino experiments}{151}{subsubsection.4.5.3}
\contentsline {subsubsection}{\numberline {4.5.4}Oscillation experiments as probes of the NSI}{154}{subsubsection.4.5.4}
\contentsline {paragraph}{\numberline {4.5.4.1}NSI and oscillations: generalities}{154}{paragraph.4.5.4.1}
\contentsline {paragraph}{\numberline {4.5.4.2}NSI and solar neutrinos}{155}{paragraph.4.5.4.2}
\contentsline {paragraph}{\numberline {4.5.4.3}NSI and atmospheric neutrinos}{158}{paragraph.4.5.4.3}
\contentsline {paragraph}{\numberline {4.5.4.4}Combined analysis of the atmospheric and K2K data}{160}{paragraph.4.5.4.4}
\contentsline {subsubsection}{\numberline {4.5.5}The role of MINOS}{161}{subsubsection.4.5.5}
\contentsline {paragraph}{\numberline {4.5.5.1}MINOS: first data release}{161}{paragraph.4.5.5.1}
\contentsline {paragraph}{\numberline {4.5.5.2}MINOS: projections for the future}{163}{paragraph.4.5.5.2}
\contentsline {paragraph}{\numberline {4.5.5.3}Summary}{165}{paragraph.4.5.5.3}
\contentsline {subsubsection}{\numberline {4.5.6}Complementarity of long and short baseline experiments}{165}{subsubsection.4.5.6}
\contentsline {section}{\numberline {5}Performance of proposed future long-baseline neutrino oscillation facilities}{166}{section.5}
\contentsline {subsection}{\numberline {5.1}Introduction}{166}{subsection.5.1}
\contentsline {subsubsection}{\numberline {5.1.1}Definition of observables}{169}{subsubsection.5.1.1}
\contentsline {subsection}{\numberline {5.2}The physics potential of super-beams}{170}{subsection.5.2}
\contentsline {subsubsection}{\numberline {5.2.1}The super-beam concept}{170}{subsubsection.5.2.1}
\contentsline {subsubsection}{\numberline {5.2.2}T2K and T2HK }{171}{subsubsection.5.2.2}
\contentsline {subsubsection}{\numberline {5.2.3}The SPL}{171}{subsubsection.5.2.3}
\contentsline {subsubsection}{\numberline {5.2.4}NO$\nu $A}{172}{subsubsection.5.2.4}
\contentsline {subsubsection}{\numberline {5.2.5}Wide-band super-beam}{173}{subsubsection.5.2.5}
\contentsline {subsubsection}{\numberline {5.2.6}Physics at a super-beam facility}{173}{subsubsection.5.2.6}
\contentsline {subsubsection}{\numberline {5.2.7}The Water \v Cerenkov Detector}{174}{subsubsection.5.2.7}
\contentsline {subsubsection}{\numberline {5.2.8}Backgrounds and efficiencies}{175}{subsubsection.5.2.8}
\contentsline {subsubsection}{\numberline {5.2.9}The super-beam performance}{176}{subsubsection.5.2.9}
\contentsline {subsubsection}{\numberline {5.2.10}The $\theta _{13}$ discovery potential}{176}{subsubsection.5.2.10}
\contentsline {subsubsection}{\numberline {5.2.11}CP-violation discovery potential}{178}{subsubsection.5.2.11}
\contentsline {subsubsection}{\numberline {5.2.12}Maximal $\theta _{23}$ exclusion potential}{178}{subsubsection.5.2.12}
\contentsline {subsubsection}{\numberline {5.2.13}Sensitivity to the atmospheric parameters}{180}{subsubsection.5.2.13}
\contentsline {subsubsection}{\numberline {5.2.14}Sensitivities to the mass hierarchy and the $\theta _{23}$ octant}{182}{subsubsection.5.2.14}
\contentsline {subsubsection}{\numberline {5.2.15}Combination with atmospheric neutrino measurements}{183}{subsubsection.5.2.15}
\contentsline {subsubsection}{\numberline {5.2.16}Super-Beam associated with a beta-beam}{185}{subsubsection.5.2.16}
\contentsline {subsubsection}{\numberline {5.2.17}Super-Beam associated with the Neutrino Factory}{185}{subsubsection.5.2.17}
\contentsline {subsection}{\numberline {5.3}The physics potential of beta-beam facilities}{187}{subsection.5.3}
\contentsline {subsubsection}{\numberline {5.3.1}Beta-beam setups}{187}{subsubsection.5.3.1}
\contentsline {subsubsection}{\numberline {5.3.2}The low-energy beta-beam: LE$\mathop {\beta \beta }$}{189}{subsubsection.5.3.2}
\contentsline {subsubsection}{\numberline {5.3.3}High-energy beta-beams: HE$\mathop {\beta \beta }$}{189}{subsubsection.5.3.3}
\contentsline {subsubsection}{\numberline {5.3.4}Ion production and $\nu $ fluxes}{189}{subsubsection.5.3.4}
\contentsline {subsubsection}{\numberline {5.3.5} Detector technology}{191}{subsubsection.5.3.5}
\contentsline {subsubsection}{\numberline {5.3.6}Water \v Cerenkov}{192}{subsubsection.5.3.6}
\contentsline {subsubsection}{\numberline {5.3.7}NO$\nu $A-like detector}{194}{subsubsection.5.3.7}
\contentsline {subsubsection}{\numberline {5.3.8}Atmospheric backgrounds}{194}{subsubsection.5.3.8}
\contentsline {subsubsection}{\numberline {5.3.9}Analysis of performance and optimisation}{195}{subsubsection.5.3.9}
\contentsline {subsubsection}{\numberline {5.3.10}Sensitivity to $\theta _{13}$}{196}{subsubsection.5.3.10}
\contentsline {subsubsection}{\numberline {5.3.11}Sensitivity to CP violation}{197}{subsubsection.5.3.11}
\contentsline {subsubsection}{\numberline {5.3.12}Sensitivity to the discrete ambiguities}{197}{subsubsection.5.3.12}
\contentsline {subsubsection}{\numberline {5.3.13}Measurement of $\theta _{13}$ and $\delta $}{198}{subsubsection.5.3.13}
\contentsline {subsubsection}{\numberline {5.3.14}Towards an optimal beta-beam setup}{198}{subsubsection.5.3.14}
\contentsline {subsubsection}{\numberline {5.3.15}Combination with atmospheric data}{198}{subsubsection.5.3.15}
\contentsline {subsubsection}{\numberline {5.3.16}An associated super-beam}{201}{subsubsection.5.3.16}
\contentsline {subsubsection}{\numberline {5.3.17}Combination of different ions}{201}{subsubsection.5.3.17}
\contentsline {subsubsection}{\numberline {5.3.18}Higher $\gamma $ ?}{202}{subsubsection.5.3.18}
\contentsline {subsubsection}{\numberline {5.3.19}Higher fluxes ?}{203}{subsubsection.5.3.19}
\contentsline {subsubsection}{\numberline {5.3.20}Monocromatic $e$-capture beams}{204}{subsubsection.5.3.20}
\contentsline {subsection}{\numberline {5.4}Optimisation and physics potential of a Neutrino Factory oscillation experiment}{205}{subsection.5.4}
\contentsline {subsubsection}{\numberline {5.4.1}The Neutrino Factory setup}{207}{subsubsection.5.4.1}
\contentsline {paragraph}{\numberline {5.4.1.1}Magnetised Iron Detector (MID): the `golden channel'}{208}{paragraph.5.4.1.1}
\contentsline {paragraph}{\numberline {5.4.1.2}Emulsion Cloud Chamber (ECC): the `silver channel'}{210}{paragraph.5.4.1.2}
\contentsline {paragraph}{\numberline {5.4.1.3}Liquid Argon Detector (LAr): the `platinum' channel}{211}{paragraph.5.4.1.3}
\contentsline {subsubsection}{\numberline {5.4.2}Physics potential of the golden channel}{213}{subsubsection.5.4.2}
\contentsline {paragraph}{\numberline {5.4.2.1}$\theta _{13}$-sensitivity}{214}{paragraph.5.4.2.1}
\contentsline {paragraph}{\numberline {5.4.2.2}CP-discovery potential}{217}{paragraph.5.4.2.2}
\contentsline {paragraph}{\numberline {5.4.2.3}Sensitivity to the mass hierarchy}{218}{paragraph.5.4.2.3}
\contentsline {paragraph}{\numberline {5.4.2.4}Measurement of the atmospheric parameters}{220}{paragraph.5.4.2.4}
\contentsline {paragraph}{\numberline {5.4.2.5}Sensitivity to maximal $\theta _{23}$ and the octant-discovery potential}{223}{paragraph.5.4.2.5}
\contentsline {paragraph}{\numberline {5.4.2.6}Optimisation for large $\qopname \relax o{sin}^2 2 \theta _{13} $}{224}{paragraph.5.4.2.6}
\contentsline {subsubsection}{\numberline {5.4.3}Solving degeneracies}{226}{subsubsection.5.4.3}
\contentsline {paragraph}{\numberline {5.4.3.1}Combining baselines}{227}{paragraph.5.4.3.1}
\contentsline {paragraph}{\numberline {5.4.3.2}Combining channels}{228}{paragraph.5.4.3.2}
\contentsline {paragraph}{\numberline {5.4.3.3}Improved detector}{233}{paragraph.5.4.3.3}
\contentsline {subsubsection}{\numberline {5.4.4}The optimal Neutrino Factory}{237}{subsubsection.5.4.4}
\contentsline {subsubsection}{\numberline {5.4.5}Low-energy neutrino factory}{241}{subsubsection.5.4.5}
\contentsline {subsection}{\numberline {5.5}Comparisons}{242}{subsection.5.5}
\contentsline {section}{\numberline {6}The potential of other alternatives}{248}{section.6}
\contentsline {subsection}{\numberline {6.1}Solar- and reactor-neutrino experiments}{248}{subsection.6.1}
\contentsline {subsubsection}{\numberline {6.1.1}The Generic $pp$ experiment}{248}{subsubsection.6.1.1}
\contentsline {subsubsection}{\numberline {6.1.2}The SK-Gd reactor experiment}{248}{subsubsection.6.1.2}
\contentsline {subsubsection}{\numberline {6.1.3}The SPMIN reactor experiment}{250}{subsubsection.6.1.3}
\contentsline {subsection}{\numberline {6.2}Atmospheric neutrino experiments}{251}{subsection.6.2}
\contentsline {subsubsection}{\numberline {6.2.1}Is the mixing angle $\theta _{23}$ maximal?}{254}{subsubsection.6.2.1}
\contentsline {subsubsection}{\numberline {6.2.2}Resolving the $\theta _{23}$ Octant Ambiguity}{255}{subsubsection.6.2.2}
\contentsline {subsubsection}{\numberline {6.2.3}Resolving the ambiguity in the neutrino-mass hierarchy}{256}{subsubsection.6.2.3}
\contentsline {subsection}{\numberline {6.3}Neutrino Mass Hierarchy from Future $0\nu \beta \beta $ Experiments}{257}{subsection.6.3}
\contentsline {subsection}{\numberline {6.4}Astrophysical methods of determining the mixing parameters}{260}{subsection.6.4}
\contentsline {subsubsection}{\numberline {6.4.1}General remarks about astrophysical neutrinos}{261}{subsubsection.6.4.1}
\contentsline {subsubsection}{\numberline {6.4.2}Unstable neutrinos arriving from cosmic distances}{262}{subsubsection.6.4.2}
\contentsline {subsubsection}{\numberline {6.4.3}Stable neutrinos and loss of coherence}{264}{subsubsection.6.4.3}
\contentsline {subsubsection}{\numberline {6.4.4}Summary }{265}{subsubsection.6.4.4}
\contentsline {section}{\numberline {7}Muon physics}{266}{section.7}
\contentsline {subsection}{\numberline {7.1}Introduction}{266}{subsection.7.1}
\contentsline {subsection}{\numberline {7.2}The Magnetic and Electric Dipole Moments of the Muon }{267}{subsection.7.2}
\contentsline {subsection}{\numberline {7.3}Search for muon number violation}{274}{subsection.7.3}
\contentsline {subsubsection}{\numberline {7.3.1}Theoretical considerations}{274}{subsubsection.7.3.1}
\contentsline {subsubsection}{\numberline {7.3.2}Model-independent analysis of rare muon processes}{274}{subsubsection.7.3.2}
\contentsline {subsection}{\numberline {7.4}Experimental prospects}{276}{subsection.7.4}
\contentsline {subsubsection}{\numberline {7.4.1}$\mu \rightarrow e \gamma $}{277}{subsubsection.7.4.1}
\contentsline {subsubsection}{\numberline {7.4.2}$\mu ^+ \to e^+e^+e^-$}{281}{subsubsection.7.4.2}
\contentsline {subsubsection}{\numberline {7.4.3}$\mu \rightarrow e$ conversion}{284}{subsubsection.7.4.3}
\contentsline {subsubsection}{\numberline {7.4.4}Muonium-anti-muonium conversion}{288}{subsubsection.7.4.4}
\contentsline {subsection}{\numberline {7.5}Normal muon decay}{292}{subsection.7.5}
\contentsline {subsubsection}{\numberline {7.5.1}Theoretical background}{292}{subsubsection.7.5.1}
\contentsline {subsubsection}{\numberline {7.5.2}Muon-lifetime measurements}{293}{subsubsection.7.5.2}
\contentsline {subsubsection}{\numberline {7.5.3}Precision measurement of the Michel parameters}{294}{subsubsection.7.5.3}
\contentsline {subsubsection}{\numberline {7.5.4}Experimental prospects}{295}{subsubsection.7.5.4}
\contentsline {subsection}{\numberline {7.6}Muon-Physics Conclusions}{296}{subsection.7.6}
\contentsline {section}{\numberline {A}Origin of the ISS and its Committees}{359}{section.A}
\contentsline {subsection}{\numberline {A.1}Origin}{359}{subsection.A.1}
\contentsline {subsection}{\numberline {A.2}Committee}{359}{subsection.A.2}