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Results in Neutrino Physics & Astrophysics : Highlights
Overview Highlights in Neutrino Oscillation Results from Atmospheric, Solar, Accelerator and Reactor Neutrino Experiments Future Directions & Projects Outlook Henry T. Wong / 王子敬 Academia Sinica / 中央研究院 @
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Neutrino Physics Road-Map
Grand Unified Theories (GUT) L(n-mass)0 Structures & Compositions of Universe mn’s;Uij’s 0 n-Oscil. mn’s n-decays 0nbb b-spect.dist. anomal. int. ………. Particle Physics Cosmology Nuclear Physics Astrophysics n’s as Probe
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Neutrino Sources n‘s everywhere: 300 per c.c.
Observed window n‘s everywhere: 300 per c.c. from sun, supernovae, cosmic rays, reactors, accelerators, astrophysical sources, & relic Big Bang …
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Cross Sections Challenges of Neutrino Experiments :
Strong Electro-magnetic Weak l(H2O) 250 light years ! Challenges of Neutrino Experiments : “How to Beat the Small Cross-Section?” i.e. By building Massive Detectors while keeping cost/background Low !
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at least as much neutrinos by mass as visible matter !
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Solar Neutrinos
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Super-Kamionkande ※ Water Cerenkov detector: 50k tons, viewed by 11,000+ =50 cm PMTs in 1000 m underground site in central Japan ※ Physics: solar n, atmospheric n , long baseline accelerator n, proton decays .. ※ Accidents (PMTs imploded) Nov 01, 50% PMT data again end of 02 !! No major deterioration in data quality
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The Sun IS Burning !! Measurement of Eccentricity of Earth’s Orbit !!!
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Sudbury Neutrino Observatory (SNO)
※ 1 kton Heavy Water Cerenkov detector: shielded by 7k ton of water viewed by 9456 PMTs located 2000 m underground in Canada. ※ Physics: Solar n …
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Solution of the “Solar Neutrino Problem”
Standard Solar Model + Standard Particle Physics Model Solution of the “Solar Neutrino Problem”
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Atmospheric Neutrinos Up-Down Asymmetry & Deficit
nm disappearing, ne OK, Strong evidence : > 15s Better fits for nt appearing Up-Down Asymmetry & Deficit
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KEK-SuperK (K2K) Accelerator n Flight path 250 km
Deficit of nm at far detector spectral distortion
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KamLAND Long Baseline Reactor n ave. flight path of 160 km
(sensitive to 20% of world’s reactors !) ave. flight path of 160 km 1 kton liquid scintillator in old Kamiokande site probe “LMA” for solar n historical results only 5 years from approved !!!!
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A “By-Product” : Earth’s Radiogenic Power :
Thermal measurements : 42 TW Geophysical Model : 16 TW KamLAND measurement : < 60 TW
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Neutrino Oscillations (in 2-family language)
Neutrinos produced & detected as ne, nm , nt (“flavor eigenstates”) Propagate as n1 , n2 (“mass eigenstates”) Probability of producingνe & detecting as νe : Matter Effect : Origin – ne+e (CC+NC) Vs nm +e(NC) 3 families at resonance
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Dm2 – : Summary 2002 PDG 2000: SK atm. n SNO solar n
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2004 K2K : Consistent Checks to atm. n SK
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+ observations of L/E oscillation signatures from SK atm-n & KamLAND (averaged)…..
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Three Families of Neutrino Mixing
The Maki-Nakagawa-Sakata (MNS) matrix : Q13 : crucial unknown towards CP-studies Possible CP Violation in n Sector:
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Normal Hierarchy: Dm232>0 Inverted Hierarchy: Dm232<0
Neutrino Mass Structures : Normal Vs Inverted Hierarchy ?? Quasi-Degenerate Vs Hierarchical ?? Dirac Vs Majorana ?? Dm2atm Dm2 Dm2 Normal Hierarchy: Dm232>0 Inverted Hierarchy: Dm232<0 0 = ?
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Deeper Physical Questions ………..
In particular : Is q12+qCabbibo = p/4 ? Is q23=p/4 ? Is q13 = 0 ? …….. Mixing angles may reveal deeper/higher energy scale & symmetry principles
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neutrino mass structures may reveal GUTs scale physics (e. g
neutrino mass structures may reveal GUTs scale physics (e.g. See-Saw Mechanisms) :
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Future Experimental Projects
Long baseline accelerator/reactor experiments (NuMI, CNGS, T2K, q13 ……) ※Detailed studies of mixing matrices by oscillation studies 0nbb experiments ※ Distinguish mass hierarchy, fix absolute mass scales Direct mass searches in b-decay ※ Probe degenerate mass structures Neutrino properties (e.g. magnetic moments studies…) ※ How neutrino interacts/couples with outside world Neutrino from sky and earth ※ do astronomy/earth science with neutrino sources, understand roles of neutrinos in astrophysics/geophysics
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Long Baseline Accelerator Neutrino Projects :
730 km NuMI MINOS CNGS Icarus/OPERA
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0nbb Candidate Isotopes
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Neutrino Mass Measurements
0nbb decay: b decay kinematics: microcalorimeters MAC-E spectrometers cosmology & structure formation astrophysics: SN ToF measurements 3H NEMO3 LNGS ´90-´03 (71.7 kg×y) |mee|= eV D.N. Spergel et al: Smn < 0.69 eV (95%CL) S.W. Allen et al: Smn = 0.56 eV (best fit) SuperK, SNO, OMNIS + grav.waves: potential for ~1eV sensitivity? 187Re 2nbb
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IceCube High Energy Neutrino Telescope
e.g. Volume ~km3 !!
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TEXONO Research Program in Taiwan
KS NPS-II : 2 cores 2.9 GW KS n Lab: 28 m from core#1
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Reactor Neutrino Interaction Cross-Sections
On-Going Data Taking: SM s(ne) T > 2 MeV R&D : Coh. (nN) T < 1 keV Results & More Data: mn(ne) T ~ keV
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min. 700 m of rock overburden
TEXONO Y2L Install 5 g ULB-ULEGe at Y2L on January 2005 Study background and feasibility for CDM searches may evolve into a full-scale (1 kg) CDM experiment Yangyang (襄陽) Lab (Y2L) min. 700 m of rock overburden
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Sensitivity Plot for CDM-WIMP search with
1 kg ULEGe at 100 eV threshold ………
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Summary & Outlook Neutrinos are important but strange objects
history of n physics full of surprises ! Strong evidenceS of massive n’s & finite mixings Physics Beyond the Standard Model ! More experiments & projects coming up EVEN MORE EXCITEMENT !
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