Results in Neutrino Physics & Astrophysics : Highlights

1. Henry T. Wong / 王子敬 Academia Sinica / 中央研究院 @ Results in Neutrino Physics & Astrophysics :Highlights • Overview • Highlights in Neutrino Oscillation Results from Atmospheric, Solar, Accelerator and Reactor Neutrino Experiments • Future Directions & Projects • Outlook

2. 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

3. n‘s everywhere: 300 per c.c. from sun, supernovae, cosmic rays, reactors, accelerators, astrophysical sources, & relic Big Bang … Observed window Neutrino Sources

4. Challenges of Neutrino Experiments : “How to Beat the Small Cross-Section?” i.e.By building Massive Detectors  while keeping cost/background Low ! Cross Sections Strong Electro-magnetic Weak l(H2O)  250 light years !

5. at least as much neutrinos by mass as visible matter !

6. Solar Neutrinos

7. 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

8. Measurement of Eccentricity of Earth’s Orbit !!! The Sun IS Burning !!

9. 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 …

11. Standard Solar Model + Standard Particle Physics Model Solution of the “Solar Neutrino Problem”

13. nm disappearing, ne OK, • Strong evidence : > 15s • Better fits for nt appearing Atmospheric Neutrinos Up-Down Asymmetry & Deficit

14. KEK-SuperK (K2K) Accelerator n Flight path 250 km Deficit of nm at far detector spectral distortion

15. KamLAND • Long Baseline Reactor n  (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 !!!!

17. A “By-Product” : • Earth’s Radiogenic Power : • Thermal measurements : 42 TW • Geophysical Model : 16 TW • KamLAND measurement : < 60 TW

18. Neutrino Oscillations(in 2-family language) • Neutrinos produced & detected as ne, nm , nt(“flavoreigenstates”) • Propagate as n1 ,n2 (“mass eigenstates”) • Probability of producingνe& detecting as νe : • Matter Effect : Origin – ne+e (CC+NC) Vs nm +e(NC) 3families at resonance

19. Dm2 –  : Summary 2002 PDG 2000: SK atm. n SNO solar n

20. 2004 K2K : Consistent Checks to atm. n SK

22. + observations of L/E oscillation signatures from SK atm-n & KamLAND (averaged)…..

24. Three Families of Neutrino Mixing The Maki-Nakagawa-Sakata (MNS) matrix : Q13 : crucial unknown towards CP-studies Possible CP Violation in n Sector:

25. Dm2 0 = ? Dm2atm Dm2 Normal Hierarchy: Dm232>0 Inverted Hierarchy: Dm232<0 Neutrino Mass Structures : • Normal Vs Inverted Hierarchy ?? • Quasi-Degenerate Vs Hierarchical ?? • Dirac Vs Majorana ??

26. 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

27. neutrino mass structures may reveal GUTs scale physics (e.g. See-Saw Mechanisms) :

28. 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 ※Probedegenerate 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

29. Long Baseline Accelerator Neutrino Projects : 730 km NuMI  MINOS CNGS  Icarus/OPERA

30. Candidate Isotopes 0nbb

31. cosmology & structure formation astrophysics: SN ToF measurements 0nbb decay: b decay kinematics: microcalorimeters MAC-E spectrometers NEMO3 76Ge @ LNGS ´90-´03 (71.7 kg×y) 2nbb D.N. Spergel et al: Smn < 0.69 eV (95%CL) S.W. Allen et al: Smn = 0.56 eV (best fit) |mee|=0.44+0.13-0.2 eV 187Re 3H SuperK, SNO, OMNIS + grav.waves: potential for ~1eV sensitivity? Neutrino Mass Measurements

33. IceCube High Energy Neutrino Telescope e.g. Volume ~km3 !!

34. TEXONO Research Program in Taiwan KS NPS-II : 2 cores  2.9 GW KS nLab: 28 m from core#1

35. 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 ~ 1-100 keV

36. Yangyang (襄陽) Lab (Y2L) min. 700 m of rock overburden TEXONO  KIMS @ 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

37. Sensitivity Plot for CDM-WIMP search with 1 kg ULEGe at 100 eV threshold ………

38. 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 !