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1、粒子物理规划及 未来的中微子实验,王贻芳 南昌，2010 高能物理年会,Particle physics: problems and methods,Standard Model: Higgs,High energy accelerators,Beyond Standard Model ? SUSY, Extra-dimensions. Compositeness, ,Neutrino properties: mass, oscillation, magnetic moment ? Majorana ?,Cosmology related problems: antimatter(CP) ?
2、Dark matter ? Relic-neutrinos, Monopoles ? Axions ? ,Details of SM (EW & QCD) : precision test, Confinement, Glueballs ? spectroscopy of particles,High intensity accelerators,Underground experiments,Surface experiments,Space experiments,High energy accelerators,High intensity accelerators,Undergroun
3、d experiments,Surface experiments,Space experiments,Tevetran: D0 CDF LHC ATLAS CMS ILC,Flavor phys.: BELLE(II) - b DAFNE s LHCb PANDA High den. phys: ALICE J-PARC n osc: T2K Minos Project-X,n osc. : SuperK KamLAND bb decay: EXO Cuore Gerda Dark matter: Xmass Xenon COUPP Astronomy Monopole Proton dec
4、ay,Cosmic-rays HESS MAGIC AUGER CTA mass Katrin n mag. Mom. TEXONO Grav. Wave Relic n Axions, ,Anti-matter/ dark matter: PAMELA FERMI AMS ATIC Asrtophysics: Integral Hubble WMAP Planck,Participate: ATLAS, CMS,Flavor phys.: BESIII - c,n osc. : Daya Bay,Cosmic-rays Yang-Ba-Jin,Asrtophysics: HXMT,Exper
5、iments in the world and at home,高能物理未来发展的基本思路,High energy accelerators 积极参加国际合作 High intensity accelerators 充分利用BESIII，取得国际一流的成果 寻机建造下一代加速器 Underground experiments 充分利用大亚湾，取得国际一流的成果 准备建造下一代中微子实验 寻机建造新的实验：暗物质、bb decay、质子衰变、。 Surface experiments 充分利用ASg & ARGO，取得国际一流的成果 积极准备建设LHAASO Space experiments
6、尽快完成HXMT，取得国际一流的成果 寻机建造新的实验：宇宙线、天体物理、暗物质、。,时间安排,十二五 前期建设的丰收期 取得重大国际影响的成果 基础能力建设 达到国际先进水平 未来项目的准备与预研 具有国际竞争力 十三五 ：重要的建设项目 下一代中微子实验：大亚湾二期 地下实验：暗物质、bb decay、质子衰变、。 空间实验：宇宙线、天体物理、暗物质、。 十四五：重大建设项目 下一代加速器,5,每个新项目必须回答以下问题： 1）为什么（与其它可能的项目比较：科学目标、经费。） 2）怎么做（概念设计、国际竞争力、科学意义、经费、技术、进度、风 险。） 3）R&D（问题、技术、方案、计划。）,
7、Neutrino oscillations: What we know and what we dont know,A mixing matrix:,Atmospheric,Solar,Majorana phase,CP phase & q13,Unknowns in neutrino oscillation: q13 , mass hierarchy, CP phase d + Majorana phase,下一代中微子实验：大亚湾二期,中微子振荡：中微子研究的中心 中微子振荡三个未解决的问题： 寻找第三种振荡，用q13表示 大亚湾中微子实验 质量顺序问题 大亚湾中微子实验二期 CP对称破缺
8、角 未来的加速器实验,为什么反应堆中微子： 1）加速器中微子实验：造价昂贵 （探测器+加速器） 2）双实验：造价昂贵，技术困难，风险巨大 3）中微子绝对质量测量：造价昂贵，技术困难 4）反应堆中微子实验：意义重大、风险小、条件优越、造价低、技术可行 测量磁矩：可能的未来，科学风险大 精确测量混合参数：大亚湾、大亚湾二期,Best neutrino source: reactor,A powerful man-made source If not too far, more powerful than solar, atmospheric, and accelerator neutrinos A
9、 well understood source（2% 0.1%） Better than solar(5-10%), atmospheric(10%), and accelerator(5-10% 2-3% ?) neutrinos Adjustable baseline Of course, accelerator can do it also A free neutrino factory,Neutrino Mass hierarchy,Mass Hierarchy: Fundamental to the Standard Model Fundamental to models beyon
10、d SM Most GUTs predict a normal mass hierarchy a discriminator of different GUTs and/or neutrino mass models Fundamental to many issues: Matter-antimatter asymmetry via leptogenesis in specific seesaw models: hierarchy related Supernova neutrinos: collective flavor transitions due to inverted mass h
11、ierarchy Radiative corrections to mn and qij are more sensitive to the inverted hierarchy,But even more important,Dirac or Majorana ?,Neutrino oscillation: beyond SM in a way of Dirac or Majorana mode ? bb exp. may never give positive results If mass hierarchy is known, together with next generation
12、 bb exp., the neutrino Dirac or Majorana nature can be determined.,next gen. bb exp.,Measuring mass hierarchy,Long baseline accelerator neutrinos Through Matter effects Expensive, project-X/LBNE in Fermilab/BNL Atmospheric neutrinos Very weak signal Huge detector, Expensive Reactor neutrinos Method:
13、 distortion of energy spectrum Enhance signature: Transform reactor neutrino L/E spectrum to frequency regime using Fourier formalism need Sin2(2q13) 0.02 Need to know DM223,S.T. Petcov et al., PLB533(2002)94 S.Choubey et al., PRD68(2003)113006,J. Learned, PRD 78(2008)071302,12,Fourier transformatio
14、n of L/E spectrum,Frequency regime is in fact the DM2 regime enhance the visible features in DM2 regime Take DM2 32 as reference NH: DM2 31 DM2 32 , DM2 31 peak at the right of DM2 32 IH: DM2 31 DM2 32 , DM2 31 peak at the left of DM2 32,L/E spectrum,Our efforts,Clear distinctive features: FCT: NH:
15、peak before valley IH: valley before peak FST: NH: prominent peak IH: prominent valley Better than power spectrum No pre-condition of Dm223,13,L. Zhan et al., PRD78:111103,2008,Quantify Features of FCT and FST,To quantify the symmetry breaking, we define: RV/LV: amplitude of the right/left valley in
16、 FCT P/V: amplitude of the peak/valley in FST For asymmetric Pee NH: RL0 and PV0 IH: RL0 and PV0,2008-07-17,14,L. Zhan et al., PRD78:111103,2008,Baseline: 46-72 km Sin2(2q13): 0.005-0.05 Others from global fit,Two clusters of RL and PV values show the sensitivity of mass hierarchy determination,In reality,L. Zhan, et. al., Phys.Rev.D79:073007,2009,Unfortunately,
