大亞灣高能物理研究所課件

1、粒子物理規(guī)劃及未來的中微子實驗王貽芳南昌，2010 高能物理年會第1頁，共29頁。Particle physics: problems and methodsStandard Model: HiggsHigh energy acceleratorsBeyond Standard Model ? SUSY, Extra-dimensions.Compositeness, Neutrino properties: mass, oscillation, magnetic moment ? Majorana ?Cosmology related problems: antimatter(CP) ?Da

2、rk matter ?Relic-neutrinos,Monopoles ? Axions ? Details of SM (EW & QCD) : precision test, Confinement, Glueballs ? spectroscopy of particlesHigh intensity acceleratorsUnderground experimentsSurface experimentsSpaceexperiments第2頁，共29頁。High energy acceleratorsHigh intensity acceleratorsUnderground ex

3、perimentsSurface experimentsSpaceexperimentsTevetran:D0CDFLHCATLASCMSILCFlavor phys.:BELLE(II) - bDAFNE sLHCbPANDA High den. phys:ALICEJ-PARCn osc.:T2KMinosProject-Xn osc. : SuperK KamLANDbb decay: EXO Cuore GerdaDark matter: Xmass Xenon COUPP AstronomyMonopoleProton decayCosmic-raysHESSMAGICAUGERCT

4、A mass Katrinn mag. Mom. TEXONOGrav. WaveRelic nAxions, Anti-matter/ dark matter: PAMELAFERMIAMSATICAsrtophysics: IntegralHubbleWMAPPlanckParticipate:ATLAS, CMSFlavor phys.:BESIII - cn osc. :Daya BayCosmic-rays Yang-Ba-JinAsrtophysics:HXMTExperiments in the world and at home第3頁，共29頁。高能物理未來發(fā)展的基本思路Hig

5、h energy accelerators積極參加國際合作High intensity accelerators充分利用BESIII，取得國際一流的成果尋機建造下一代加速器Underground experiments充分利用大亞灣，取得國際一流的成果準備建造下一代中微子實驗尋機建造新的實驗：暗物質、bb decay、質子衰變、。Surface experiments充分利用ASg & ARGO，取得國際一流的成果積極準備建設LHAASOSpace experiments盡快完成HXMT，取得國際一流的成果尋機建造新的實驗：宇宙線、天體物理、暗物質、。第4頁，共29頁。時間安排十二五前期建設的

6、豐收期 取得重大國際影響的成果基礎能力建設 達到國際先進水平未來項目的準備與預研 具有國際競爭力十三五 ：重要的建設項目下一代中微子實驗：大亞灣二期 地下實驗：暗物質、bb decay、質子衰變、?？臻g實驗：宇宙線、天體物理、暗物質、。十四五：重大建設項目 下一代加速器5每個新項目必須回答以下問題：1）為什么（與其它可能的項目比較：科學目標、經費。）2）怎么做（概念設計、國際競爭力、科學意義、經費、技術、進度、風 險。）3）R&D（問題、技術、方案、計劃。）第5頁，共29頁。Neutrino oscillations: What we know and what we dont knowA m

7、ixing matrix: Atmospheric Solar Majorana phase CP phase & q13Unknowns in neutrino oscillation: q13 , mass hierarchy, CP phase d + Majorana phase 第6頁，共29頁。下一代中微子實驗：大亞灣二期中微子振蕩：中微子研究的中心中微子振蕩三個未解決的問題：尋找第三種振蕩，用q13表示 大亞灣中微子實驗質量順序問題 大亞灣中微子實驗二期 CP對稱破缺角 未來的加速器實驗 n1n2n3q12太陽中微子振蕩q23大氣中微子振蕩q13 ?mi ?為什么反應堆中微子：1

8、）加速器中微子實驗：造價昂貴 （探測器+加速器） 2）雙實驗：造價昂貴，技術困難，風險巨大3）中微子絕對質量測量：造價昂貴，技術困難4）反應堆中微子實驗：意義重大、風險小、條件優(yōu)越、造價低、技術可行測量磁矩：可能的未來，科學風險大精確測量混合參數(shù)：大亞灣、大亞灣二期第7頁，共29頁。Best neutrino source: reactorA powerful man-made sourceIf not too far, more powerful than solar, atmospheric, and accelerator neutrinosA well understood sourc

9、e（2% 0.1%）Better than solar(5-10%), atmospheric(10%), and accelerator(5-10% 2-3% ?) neutrinosAdjustable baselineOf course, accelerator can do it alsoA free neutrino factory第8頁，共29頁。Neutrino Mass hierarchyMass Hierarchy:Fundamental to the Standard ModelFundamental to models beyond SM Most GUTs predic

10、t a normal mass hierarchy a discriminator of different GUTs and/or neutrino mass modelsFundamental to many issues: Matter-antimatter asymmetry via leptogenesis in specific seesaw models: hierarchy related Supernova neutrinos: collective flavor transitions due to inverted mass hierarchyRadiative corr

11、ections to mn and qij are more sensitive to the inverted hierarchyBut even more important 第9頁，共29頁。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 bb exp., the n

12、eutrino Dirac or Majorana nature can be determined. next gen. bb exp.第10頁，共29頁。Measuring mass hierarchyLong baseline accelerator neutrinosThrough Matter effectsExpensive, project-X/LBNE in Fermilab/BNLAtmospheric neutrinosVery weak signalHuge detector, Expensive Reactor neutrinosMethod: distortion o

13、f energy spectrumEnhance signature: Transform reactor neutrino L/E spectrum to frequency regime using Fourier formalismneed Sin2(2q13) 0.02Need to know DM223 S.T. Petcov et al., PLB533(2002)94S.Choubey et al., PRD68(2003)113006J. Learned, PRD 78(2008)071302 第11頁，共29頁。12Fourier transformation of L/E

14、spectrum Frequency regime is in fact the DM2 regime enhance the visible features in DM2 regime Take DM2 32 as referenceNH: DM2 31 DM2 32 , DM2 31 peak at the right of DM2 32 IH: DM2 31 0 and PV0IH: RL0 and PV 90% CL:Baseline: 58 km, determined by q12Reactor power 24 GWthFlux and detector size: (250-

15、700) ktyearIdeally, sin22q13 0.02 & energy resolution 2%IF sin22q13=0.01, energy resolution 2% & 700 ktyearFor sin22q13=0.02 , energy resolution 1000 MWE 60 km from Daya BayA huge ne detector with mass 20ktcurrently the largest on is 1kt (KamLAND & LVD) 第16頁，共29頁。Scientific goal: a l0-50kt undergrou

16、nd LS detector 60km from reactor Neutrino Mass hierarchyPrecision mixing para. measurement: q12, D M212, DM231 Unitarity of the mixing matrixSupernova neutrinos =better than SuperKGeo-neutrinos =10 better than KamLANDAtmospheric neutrinos = SuperKSolar neutrinos ? High energy neutrinosPoint source:

17、GRB, AGN, BH, Diffused neutrinosHigh energy cosmic-muonsPoint source: GRB, AGN, BH, Dark matterExotics Sterile neutrinosMonopoles, Fractional charged particles, .LVD+MACRO+KamLAND+SuperK第17頁，共29頁。Precision measurement of mixing parameter Fundamental to the Standard Model and beyondSimilarities point

18、 to a Grand unification of leptons and quarksConstrain all PMNS matrix elements to 1% ! Probing Unitarity of UPMNS to 1% level !If we can spend (0.1-0.5)B$ for each B/C/superB factories to understand UCKM ( 1-2 elements for each factory), why not a super-reactor neutrino experiment( 3 elements) to u

19、nderstand UPMNS ? Current BESIII Vub25%5%Vcd7%1%Vcs16%1%Vcb5%3%Vtd36%5%Vts39%5%Current Daya Bay II Dm2125% 1% Dm22312% 1%sin2q1210% 1%Sin2q2320%-sin2q13-第18頁，共29頁。Supernova neutrinosLess than 20 events observed so far (2001 Noble prize)Assumptions:Distance: 10 kpc (our Galaxy center) Energy: 31053 e

20、rgLn the same for all typesTem. & energyMany types of events:ne + p n + e+, 3000 correlated eventsne + 12C 13B* + e+, 10-100 correlated eventsne + 12C 11N* + e-, 10-100 correlated eventsnx + 12C n+ 12C*, 600 correlated eventsnx + p n+ p, single eventsne + e- ne + e-, single eventsnx + e- n+ e-, sing

21、le eventsT(ne) = 3.5 MeV, = 11 MeVT(ne) = 5 MeV, = 16 MeVT(nx) = 8 MeV, = 25 MeV SuperK can not see these correlated events第19頁，共29頁。What to do with Supernova neutrinosEnergy spectra & fluxes of all types of neutrinos tem. and average energy of neutrinos Understand Supernovae neutrino properties: ma

22、ss, mixing, Earth tomographyNeutrino modelsArrival time of all types of neutrinos absolute neutrino mass第20頁，共29頁。Geo-neutrinos 238U, 232Th and 40K decays account for 40% of earths power, which is related to earthquakes, volcanoes, geomagnetism, plate tectonics, They are mainly from mantle and crust

23、, but not the coreSouth-china and Japan are differentGeo-neutrinos can tell 238U: 232Th good for geo-modelsOnly way looking inside the earth ?Already seen by KamLAND第21頁，共29頁。Geo-neutrinos at Daya Bay IIA factor of 10 larger than KamLAND3 years KamLAND第22頁，共29頁。探測器的概念設計Neutrino target: 20kt LS, LAB

24、based 30m(D)30m(H)Oil buffer: 6ktWater buffer: 10kt PMT: 15000 20”Cost: 1.5 B RMB第23頁，共29頁?？赡艿牡攸c：惠州或海上據(jù)大亞灣/海豐60公里熱功率 40 GW第24頁，共29頁。Technical challengesRequirements: Large detector: 10 kt LSEnergy resolution: 2%/E 2500 p.e./MeVOngoing R&D:Low cost, high QE “PMT”A new design exist, patent pending, R&D contract to be signed with manufacturetransparent LS: 15m 25mFind out tra