粒子物理規(guī)劃及未來的中微子實(shí)驗(yàn)

1、粒子物理規(guī)劃及未來的中微子實(shí)驗(yàn)王貽芳南昌，2010 高能物理年會(huì)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) ?Dark matter

2、 ?Relic-neutrinos,Monopoles ? Axions ? Details of SM (EW & QCD) : precision test, Confinement, Glueballs ? spectroscopy of particlesHigh intensity acceleratorsUnderground experimentsSurface experimentsSpaceexperimentsHigh energy acceleratorsHigh intensity acceleratorsUnderground experimentsSurface e

3、xperimentsSpaceexperimentsTevetran: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-raysHESSMAGICAUGERCTA mass Katrinn mag

4、. 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高能物理未來發(fā)展的基本思路High energy accelerators積極參加國際

5、合作High intensity accelerators充分利用BESIII，取得國際一流的成果尋機(jī)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(zhǔn)備建造下一代中微子實(shí)驗(yàn)尋機(jī)建造新的實(shí)驗(yàn)：暗物質(zhì)、bb decay、質(zhì)子衰變、。Surface experiments充分利用ASg & ARGO，取得國際一流的成果積極準(zhǔn)備建設(shè)LHAASOSpace experiments盡快完成HXMT，取得國際一流的成果尋機(jī)建造新的實(shí)驗(yàn)：宇宙線、天體物理、暗物質(zhì)、。時(shí)間安排十二五前期建設(shè)的豐收期 取得重大國際影響的成果基礎(chǔ)能力建設(shè) 達(dá)到國際先進(jìn)水平未來項(xiàng)目的準(zhǔn)

6、備與預(yù)研 具有國際競爭力十三五 ：重要的建設(shè)項(xiàng)目下一代中微子實(shí)驗(yàn)：大亞灣二期 地下實(shí)驗(yàn)：暗物質(zhì)、bb decay、質(zhì)子衰變、?？臻g實(shí)驗(yàn)：宇宙線、天體物理、暗物質(zhì)、。十四五：重大建設(shè)項(xiàng)目 下一代加速器5每個(gè)新項(xiàng)目必須回答以下問題：1）為什么（與其它可能的項(xiàng)目比較：科學(xué)目標(biāo)、經(jīng)費(fèi)。）2）怎么做（概念設(shè)計(jì)、國際競爭力、科學(xué)意義、經(jīng)費(fèi)、技術(shù)、進(jìn)度、風(fēng) 險(xiǎn)。）3）R&D（問題、技術(shù)、方案、計(jì)劃。）Neutrino oscillations: What we know and what we dont knowA mixing matrix: Atmospheric Solar Majorana phas

7、e CP phase & q13Unknowns in neutrino oscillation: q13 , mass hierarchy, CP phase d + Majorana phase 下一代中微子實(shí)驗(yàn)：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(gè)未解決的問題：尋找第三種振蕩，用q13表示 大亞灣中微子實(shí)驗(yàn)質(zhì)量順序問題 大亞灣中微子實(shí)驗(yàn)二期 CP對(duì)稱破缺角 未來的加速器實(shí)驗(yàn) n1n2n3q12太陽中微子振蕩q23大氣中微子振蕩q13 ?mi ?為什么反應(yīng)堆中微子：1）加速器中微子實(shí)驗(yàn)：造價(jià)昂貴 （探測器+加速器） 2）雙實(shí)驗(yàn)：造價(jià)昂貴，技術(shù)困難，風(fēng)險(xiǎn)巨大3）中微子絕對(duì)質(zhì)量

8、測量：造價(jià)昂貴，技術(shù)困難4）反應(yīng)堆中微子實(shí)驗(yàn)：意義重大、風(fēng)險(xiǎn)小、條件優(yōu)越、造價(jià)低、技術(shù)可行測量磁矩：可能的未來，科學(xué)風(fēng)險(xiǎn)大精確測量混合參數(shù)：大亞灣、大亞灣二期Best neutrino source: reactorA powerful man-made sourceIf not too far, more powerful than solar, atmospheric, and accelerator neutrinosA well understood source（2% 0.1%）Better than solar(5-10%), atmospheric(10%), and accel

9、erator(5-10% 2-3% ?) neutrinosAdjustable baselineOf course, accelerator can do it alsoA free neutrino factoryNeutrino Mass hierarchyMass Hierarchy:Fundamental to the Standard ModelFundamental to models beyond SM Most GUTs predict a normal mass hierarchy a discriminator of different GUTs and/or neutr

10、ino 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 corrections to mn and qij are more sensitive to the inverted hierarchyBut ev

11、en 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 bb exp., the neutrino Dirac or Majorana nature can be determined. next gen. bb exp.Measuring ma

12、ss hierarchyLong baseline accelerator neutrinosThrough Matter effectsExpensive, project-X/LBNE in Fermilab/BNLAtmospheric neutrinosVery weak signalHuge detector, Expensive Reactor neutrinosMethod: distortion of energy spectrumEnhance signature: Transform reactor neutrino L/E spectrum to frequency re

13、gime 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 12Fourier transformation of L/E spectrum Frequency regime is in fact the DM2 regime enhance the visible features in DM2 regime Take D

14、M2 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: (250-700) ktyearIdeally, sin22q13 0.02 & energy resolution 2%IF sin22q13=0.01, energy resolution 2% & 700

15、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) Scientific goal: a l0-50kt underground LS detector 60km from reactor Neutrino Mass hierarchyPrecision mixing para. measurement: q12, D M212, DM231

16、Unitarity of the mixing matrixSupernova neutrinos =better than SuperKGeo-neutrinos =10 better than KamLANDAtmospheric neutrinos = SuperKSolar neutrinos ? High energy neutrinosPoint source: GRB, AGN, BH, Diffused neutrinosHigh energy cosmic-muonsPoint source: GRB, AGN, BH, Dark matterExotics Sterile

17、neutrinosMonopoles, Fractional charged particles, .LVD+MACRO+KamLAND+SuperKPrecision measurement of mixing parameter Fundamental to the Standard Model and beyondSimilarities point to a Grand unification of leptons and quarksConstrain all PMNS matrix elements to 1% ! Probing Unitarity of UPMNS to 1%

18、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 understand UPMNS ? Current BESIII Vub25%5%Vcd7%1%Vcs16%1%Vcb5%3%Vtd36%5%Vts39%5%Current Daya Bay II Dm2125% 1% Dm22312% 1%

19、sin2q1210% 1%Sin2q2320%-sin2q13-Supernova neutrinosLess than 20 events observed so far (2001 Noble prize)Assumptions:Distance: 10 kpc (our Galaxy center) Energy: 31053 ergLn the same for all typesTem. & energyMany types of events:ne + p n + e+, 3000 correlated eventsne + 12C 13B* + e+, 10-100 correl

20、ated 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-, single eventsT(ne) = 3.5 MeV, = 11 MeVT(ne) = 5 MeV, = 16 MeVT(nx) = 8 MeV, = 25 MeV SuperK can not see these correlated eventsWhat to

21、do with Supernova neutrinosEnergy spectra & fluxes of all types of neutrinos tem. and average energy of neutrinos Understand Supernovae neutrino properties: mass, mixing, Earth tomographyNeutrino modelsArrival time of all types of neutrinos absolute neutrino massGeo-neutrinos 238U, 232Th and 40K dec

22、ays account for 40% of earths power, which is related to earthquakes, volcanoes, geomagnetism, plate tectonics, They are mainly from mantle and crust, but not the coreSouth-china and Japan are differentGeo-neutrinos can tell 238U: 232Th good for geo-modelsOnly way looking inside the earth ?Already s

23、een by KamLANDGeo-neutrinos at Daya Bay IIA factor of 10 larger than KamLAND3 years KamLAND探測器的概念設(shè)計(jì)Neutrino target: 20kt LS, LAB based 30m(D)30m(H)Oil buffer: 6ktWater buffer: 10kt PMT: 15000 20”Cost: 1.5 B RMB可能的地點(diǎn)：惠州或海上據(jù)大亞灣/海豐60公里熱功率 40 GWTechnical challengesRequirements: Large detector: 10 kt LSE

24、nergy 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 traces which absorb light, remove it from production R&D program: 3 yearsUseful for many future projectsSupport already from IHEPNow: 1kt250 p.e./MeV基于LAB的液體閃爍體研究測量LAB成分：4.5% 雜質(zhì)利用量子化學(xué)的計(jì)算，估計(jì)、尋找吸收可見光的雜質(zhì)初步測量雜質(zhì)在L