粒子物理規(guī)劃及未來的中微子實驗

1、粒子物理規(guī)劃及粒子物理規(guī)劃及未來的中微子實驗未來的中微子實驗王貽芳王貽芳南昌，南昌，2010 高能物理年會高能物理年會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:

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

3、ground experimentsSurface experimentsSpaceexperimentsTevetran:D0CDFLHCATLASCMSILCFlavor phys.:BELLE(II) - bDAFNE sLHCbPANDA High den. phys:ALICEJ-PARCn n osc.:T2KMinosProject-Xn n osc. : SuperK KamLANDbb bb decay: EXO Cuore GerdaDark matter: Xmass Xenon COUPPn AstronomyMonopoleProton decayCosmic-ray

4、sHESSMAGICAUGERCTAn mass Katrinn n mag. Mom. TEXONOGrav. WaveRelic n nAxions, Anti-matter/ dark matter: PAMELAFERMIAMSATICAsrtophysics: IntegralHubbleWMAPPlanckParticipate:ATLAS, CMSFlavor phys.:BESIII - cn n osc. :Daya BayCosmic-rays Yang-Ba-JinAsrtophysics:HXMTExperiments in the world and at home高

5、能物理未來發(fā)展的基本思路高能物理未來發(fā)展的基本思路 High energy accelerators 積極參加國際合作積極參加國際合作 High intensity accelerators 充分利用充分利用BESIII，取得國際一流的成果，取得國際一流的成果 尋機(jī)建造下一代加速器尋機(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驗準(zhǔn)備建造下一代中微子實驗 尋機(jī)建造新的實驗：暗物質(zhì)、尋機(jī)建造新的實驗：暗物質(zhì)、bb bb decay、質(zhì)子衰變、。、質(zhì)子衰變、。 Surface expe

6、riments 充分利用充分利用ASg g & ARGO，取得國際一流的成果，取得國際一流的成果 積極準(zhǔn)備建設(shè)積極準(zhǔn)備建設(shè)LHAASO Space experiments 盡快完成盡快完成HXMT，取得國際一流的成果，取得國際一流的成果 尋機(jī)建造新的實驗：宇宙線、天體物理、暗物質(zhì)、。尋機(jī)建造新的實驗：宇宙線、天體物理、暗物質(zhì)、。時間安排時間安排 十二五十二五 前期建設(shè)的豐收期前期建設(shè)的豐收期 取得重大國際影響的成果取得重大國際影響的成果 基礎(chǔ)能力建設(shè)基礎(chǔ)能力建設(shè) 達(dá)到國際先進(jìn)水平達(dá)到國際先進(jìn)水平 未來項目的準(zhǔn)備與預(yù)研未來項目的準(zhǔn)備與預(yù)研 具有具有國際競爭力國際競爭力 十三五十三五 ：重要的建設(shè)

7、項目：重要的建設(shè)項目 下一代中微子實驗：大亞灣二期下一代中微子實驗：大亞灣二期 地下實驗：暗物質(zhì)、地下實驗：暗物質(zhì)、bb bb decay、質(zhì)子衰變、。、質(zhì)子衰變、。 空間實驗：宇宙線、天體物理、暗物質(zhì)、。空間實驗：宇宙線、天體物理、暗物質(zhì)、。 十四五：重大建設(shè)項目十四五：重大建設(shè)項目 下一代加速器下一代加速器5每個新項目必須回答以下問題：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(xué)目標(biāo)、經(jīng)費(fèi)。）為什么（與其它可能的項目比較：科學(xué)目標(biāo)、經(jīng)費(fèi)。）2）怎么做（概念設(shè)計、國際競爭力、科學(xué)意義、經(jīng)費(fèi)、技術(shù)、進(jìn)度、風(fēng)）怎么做（概念設(shè)計、國際競爭力、科學(xué)意義、經(jīng)費(fèi)、技術(shù)、進(jìn)度、風(fēng) 險

8、。）險。）3）R&D（問題、技術(shù)、方案（問題、技術(shù)、方案、計劃。）、計劃。）Neutrino oscillations: What we know and what we dont know A mixing matrix: Atmospheric Solar Majorana phase CP phase & q q13 Unknowns in neutrino oscillation: q q13 , mass hierarchy, CP phase d d + Majorana phase 下一代中微子實驗：大亞灣二期下一代中微子實驗：大亞灣二期 中微子振蕩：中微子研究的中心中微子振蕩：

9、中微子研究的中心 中微子振蕩三個未解決的問題：中微子振蕩三個未解決的問題：尋找第三種振蕩，用尋找第三種振蕩，用q q13表示表示 大亞灣中微子實驗大亞灣中微子實驗質(zhì)量順序問題質(zhì)量順序問題 大亞灣中微子實驗二期大亞灣中微子實驗二期 CP對稱破缺角對稱破缺角 未來的加速器實驗未來的加速器實驗 n n1n n2n n3q q12太陽中微子振蕩太陽中微子振蕩q q23大氣中微子振蕩大氣中微子振蕩q q13 ?mi ?為什么反應(yīng)堆中微子：為什么反應(yīng)堆中微子：1）加速器中微子實驗：造價昂貴）加速器中微子實驗：造價昂貴 （探測器（探測器+加速器）加速器） 2）雙）雙實驗：造價昂貴，技術(shù)困難，風(fēng)險巨大實驗：造

10、價昂貴，技術(shù)困難，風(fēng)險巨大3）中微子絕對質(zhì)量測量：造價昂貴，技術(shù)困難）中微子絕對質(zhì)量測量：造價昂貴，技術(shù)困難4）反應(yīng)堆中微子實驗：意義重大、風(fēng)險小、條件優(yōu)越、造價低、技術(shù)可行）反應(yīng)堆中微子實驗：意義重大、風(fēng)險小、條件優(yōu)越、造價低、技術(shù)可行l(wèi)測量磁矩：可能的未來，科學(xué)風(fēng)險大測量磁矩：可能的未來，科學(xué)風(fēng)險大l精確測量混合參數(shù)：大亞灣、大亞灣二期精確測量混合參數(shù)：大亞灣、大亞灣二期Best neutrino source: reactor A powerful man-made source If not too far, more powerful than solar, atmospheric,

11、 and accelerator neutrinos A 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 factoryNeutrino Mass hierarchy Mass Hierarchy: Fundamental to the Standard Model

12、Fundamental to models beyond 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 transit

13、ions due to inverted mass hierarchy Radiative corrections to mn n and q qij are more sensitive to the inverted hierarchyBut even more important Dirac or Majorana ? Neutrino oscillation: beyond SM in a way of Dirac or Majorana mode ? bb bb exp. may never give positive results If mass hierarchy is kno

14、wn, together with next generation bb bb exp., the neutrino Dirac or Majorana nature can be determined. next gen. bb 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 detecto

15、r, Expensive Reactor neutrinos Method: distortion of energy spectrum Enhance signature: Transform reactor neutrino L/E spectrum to frequency regime using Fourier formalism need Sin2(2q q13) 0.02 Need to know D DM223 S.T. Petcov et al., PLB533(2002)94S.Choubey et al., PRD68(2003)113006J. Learned, PRD

16、 78(2008)071302 12Fourier transformation of L/E spectrum Frequency regime is in fact the D DM2 regime enhance the visible features in D DM2 regime Take D DM2 32 as reference NH: D DM2 31 D DM2 32 , D DM2 31 peak at the right of D DM2 32 IH: D DM2 31 0 and PV0 IH: RL0 and PV 90% CL: Baseline: 58 km,

17、determined by q q12 Reactor power 24 GWth Flux and detector size: (250-700) kt year Ideally, sin22q q13 0.02 & energy resolution 2% IF sin22q q13=0.01, energy resolution 2% & 700 kt year For sin22q q13=0.02 , energy resolution 1000 MWE 60 km from Daya Bay A huge n ne detector with mass 20kt currentl

18、y the largest on is 1kt (KamLAND & LVD) Scientific goal: a l0-50kt underground LS detector 60km from reactor 1. Neutrino Mass hierarchy2. Precision mixing para. measurement: q q12, D D M212, D DM231 Unitarity of the mixing matrix3. Supernova neutrinos =better than SuperK4. Geo-neutrinos = 10 better

19、than KamLAND5. Atmospheric neutrinos = SuperK6. Solar neutrinos ? 7. High energy neutrinos1.Point source: GRB, AGN, BH, 2.Diffused neutrinos8. High energy cosmic-muons1.Point source: GRB, AGN, BH, 2.Dark matter9. Exotics 1.Sterile neutrinos2.Monopoles, Fractional charged particles, .LVD+MACRO+KamLAN

20、D+SuperKPrecision measurement of mixing parameter Fundamental to the Standard Model and beyond Similarities point to a Grand unification of leptons and quarks Constrain 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

21、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 D Dm2125% 1% D Dm22312% 1%sin2q q1210% 1%Sin2q q2320%-sin2q q13 -Supernova neutrinos Le

22、ss than 20 events observed so far (2001 Noble prize) Assumptions: Distance: 10 kpc (our Galaxy center) Energy: 3 1053 erg Ln n the same for all types Tem. & energyMany types of events:n ne + p n + e+, 3000 correlated eventsn ne + 12C 13B* + e+, 10-100 correlated eventsn ne + 12C 11N* + e-, 10-100 co

23、rrelated eventsn nx + 12C n n+ 12C*, 600 correlated eventsn nx + p n n+ p, single eventsn ne + e- n ne + e-, single eventsn nx + e- n n+ e-, single eventsT(n ne) = 3.5 MeV, = 11 MeVT(n ne) = 5 MeV, = 16 MeVT(n nx) = 8 MeV, = 25 MeV SuperK can not see these correlated eventsWhat to do with Supernova

24、neutrinos Energy spectra & fluxes of all types of neutrinos tem. and average energy of neutrinos Understand Supernovae neutrino properties: mass, mixing, Earth tomography Neutrino models Arrival time of all types of neutrinos absolute neutrino massGeo-neutrinos 238U, 232Th and 40K decays account for

25、 40% of earths power, which is related to earthquakes, volcanoes, geomagnetism, plate tectonics, They are mainly from mantle and crust, but not the core South-china and Japan are different Geo-neutrinos can tell 238U: 232Th good for geo-models Only way looking inside the earth ?Already seen by KamLA

26、NDGeo-neutrinos at Daya Bay II A factor of 10 larger than KamLAND3 years KamLAND探測器的概念設(shè)計探測器的概念設(shè)計 Neutrino target: 20kt LS, LAB based 30m(D) 30m(H) Oil buffer: 6kt Water buffer: 10kt PMT: 15000 20” Cost: 1.5 B RMB可能的地點(diǎn)：惠州或海上可能的地點(diǎn)：惠州或海上據(jù)大亞灣據(jù)大亞灣/海豐海豐60公里公里熱功率熱功率 40 GWTechnical challenges Requirements:

27、Large detector: 10 kt LS Energy resolution: 2%/ E 2500 p.e./MeV Ongoing R&D: Low cost, high QE “PMT” A new design exist, patent pending, R&D contract to be signed with manufacture transparent LS: 15m 25m Find 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基于基于LAB的液體閃爍體研究的液體閃爍體研究 測量測量LAB成分：成分：4.5% 雜質(zhì)雜質(zhì) 利用量子化學(xué)的計算，估計、尋找吸收可見光的雜質(zhì)利用量子化學(xué)的計算，估計、尋找吸收可見光的雜質(zhì) 初步測量雜質(zhì)在初步測量雜質(zhì)在LAB中的比