粒子物理規(guī)劃及未來(lái)的中微子實(shí)驗(yàn)

1、粒子物理規(guī)劃及粒子物理規(guī)劃及未來(lái)的中微子實(shí)驗(yàn)未來(lái)的中微子實(shí)驗(yàn)王貽芳王貽芳南昌，南昌，2010 高能物理年會(huì)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:

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 acceleratorsU

3、nderground 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

4、-raysHESSMAGICAUGERCTAn 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 h

5、ome高能物理未來(lái)發(fā)展的基本思路高能物理未來(lái)發(fā)展的基本思路 High energy accelerators 積極參加國(guó)際合作積極參加國(guó)際合作 High intensity accelerators 充分利用充分利用BESIII，取得國(guó)際一流的成果，取得國(guó)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(guó)際一流的成果充分利用大亞灣，取得國(guó)際一流的成果 準(zhǔn)備建造下一代中微子實(shí)驗(yàn)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)、尋機(jī)建造新的實(shí)驗(yàn)：暗物質(zhì)、bb bb decay、質(zhì)子衰變、。、質(zhì)子衰變、。 Surface

6、experiments 充分利用充分利用ASg g & ARGO，取得國(guó)際一流的成果，取得國(guó)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(guó)際一流的成果，取得國(guó)際一流的成果 尋機(jī)建造新的實(shí)驗(yàn)：宇宙線(xiàn)、天體物理、暗物質(zhì)、。尋機(jī)建造新的實(shí)驗(yàn)：宇宙線(xiàn)、天體物理、暗物質(zhì)、。時(shí)間安排時(shí)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(guó)際影響的成果取得重大國(guó)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(guó)際先進(jìn)水平達(dá)到國(guó)際先進(jìn)水平 未來(lái)項(xiàng)目的準(zhǔn)備與預(yù)研未來(lái)項(xiàng)目的準(zhǔn)備與預(yù)研 具有具有國(guó)際競(jìng)爭(zhēng)力國(guó)際競(jìng)爭(zhēng)力 十三五十三

7、五 ：重要的建設(shè)項(xiàng)目：重要的建設(shè)項(xiàng)目 下一代中微子實(shí)驗(yàn)：大亞灣二期下一代中微子實(shí)驗(yàn)：大亞灣二期 地下實(shí)驗(yàn)：暗物質(zhì)、地下實(shí)驗(yàn)：暗物質(zhì)、bb bb decay、質(zhì)子衰變、。、質(zhì)子衰變、。 空間實(shí)驗(yàn)：宇宙線(xiàn)、天體物理、暗物質(zhì)、?？臻g實(shí)驗(yàn)：宇宙線(xiàn)、天體物理、暗物質(zhì)、。 十四五：重大建設(shè)項(xiàng)目十四五：重大建設(shè)項(xiàng)目 下一代加速器下一代加速器5每個(gè)新項(xiàng)目必須回答以下問(wèn)題：每個(gè)新項(xiàng)目必須回答以下問(wèn)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)。）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(guó)際競(jìng)爭(zhēng)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(jì)、國(guó)際競(jìng)爭(zhēng)力、科學(xué)意義、經(jīng)費(fèi)、技

8、術(shù)、進(jìn)度、風(fēng) 險(xiǎn)。）險(xiǎn)。）3）R&D（問(wèn)題、技術(shù)、方案（問(wèn)題、技術(shù)、方案、計(jì)劃。）、計(jì)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(shí)驗(yàn)：大亞灣二期下一代中微子實(shí)驗(yàn)：大亞灣二期 中微子振

9、蕩：中微子研究的中心中微子振蕩：中微子研究的中心 中微子振蕩三個(gè)未解決的問(wèn)題：中微子振蕩三個(gè)未解決的問(wèn)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(shí)驗(yàn)大亞灣中微子實(shí)驗(yàn)質(zhì)量順序問(wèn)題質(zhì)量順序問(wèn)題 大亞灣中微子實(shí)驗(yàn)二期大亞灣中微子實(shí)驗(yàn)二期 CP對(duì)稱(chēng)破缺角對(duì)稱(chēng)破缺角 未來(lái)的加速器實(shí)驗(yàn)未來(lái)的加速器實(shí)驗(yàn) n n1n n2n n3q q12太陽(yáng)中微子振蕩太陽(yáng)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(shí)驗(yàn)：造價(jià)昂貴）加速器中微子實(shí)驗(yàn)：造價(jià)昂貴 （探測(cè)器（探測(cè)器+加速器）加速器） 2）雙）雙實(shí)驗(yàn)：造價(jià)

10、昂貴，技術(shù)困難，風(fēng)險(xiǎn)巨大實(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)量測(cè)量：造價(jià)昂貴，技術(shù)困難）中微子絕對(duì)質(zhì)量測(cè)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）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l(wèi)測(cè)量磁矩：可能的未來(lái)，科學(xué)風(fēng)險(xiǎn)大測(cè)量磁矩：可能的未來(lái)，科學(xué)風(fēng)險(xiǎn)大l精確測(cè)量混合參數(shù)：大亞灣、大亞灣二期精確測(cè)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 sol

11、ar, atmospheric, 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

12、 Standard Model 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: collectiv

13、e flavor transitions 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

14、hierarchy is known, 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 sig

15、nal Huge detector, 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)11300

16、6J. Learned, PRD 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: B

17、aseline: 58 km, 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

18、 with mass 20kt currently 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

19、. Geo-neutrinos = 10 better 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

20、particles, .LVD+MACRO+KamLAND+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$ fo

21、r 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 D Dm2125% 1% D Dm22312% 1%sin2q q1210% 1%Sin2q q2320%-sin2q

22、 q13 -Supernova neutrinos Less 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 event

23、sn ne + 12C 11N* + e-, 10-100 correlated 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

24、eventsWhat to do with Supernova 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 23

25、8U, 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, but not the core South-china and Japan are different Geo-neutrinos can tell 238U: 232Th good for geo-models Only way looking ins

26、ide the earth ?Already seen by KamLANDGeo-neutrinos at Daya Bay II A factor of 10 larger than KamLAND3 years KamLAND探測(cè)器的概念設(shè)計(jì)探測(cè)器的概念設(shè)計(jì) 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 G

27、WTechnical challenges Requirements: 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(cè)量測(cè)量LAB成分：成分：4.5% 雜質(zhì)雜質(zhì) 利用量子化學(xué)的計(jì)算，估計(jì)、尋找吸收可見(jiàn)光的雜質(zhì)利用量子化學(xué)的計(jì)算，估計(jì)、尋找吸收可見(jiàn)光的雜質(zhì) 初步測(cè)量雜質(zhì)在初步測(cè)量雜質(zhì)在L