The Importance of Low-Energy Solar Neutrino Experiments：低能量太阳中微子实验的重要性
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– There are 3 types of neutrinos : ne , nm , nt – Neutrinos have mass and oscillate – Oscillation parameters (Dm2 and tan2q) known to ~ 30% – Neutrino masses are small
Expect sensitivity of 10-11 mB
Nuclear Physics
p-p Solar Neutrino Experiments: Physics Goals
Macintosh PICT image format is not supported
Equally sensitive to all flavours
ES Interaction
M a c in to s h P IC T im a g e fo rm a t
is n o t s u p p o rte d
• Directly observe the 99.99% of solar neutrinos that are below 5 MeV Direct test of solar models (p-p, 7Be, CNO)
• DMeetaesrumremiUnenencuterontfaitCianNrtiiOetsynin/eudtthireminseonslasprirononevuidotrefisnnaonmfliuimxxipensogrtmanat ttresixt: PresGo••efn1Cot.taN5hl%Oeispbot-fuoptrhnmseioneSlgaauirsnsp1u’ncs5-rrp’%eesunctteihora73gel1B5yif%ne%lisafivfrprosorC1trme0N1c0c0O%ito8shmiyeorCpnc86oNoBi%snnOivteicocytncilvee stage Witah• Pmproeosvdeiendlte-sintedset pofe1nin2di%teianltm8me%taanllnic1ei0try0%of the4%Sun
M a c in t o s h
P IC T
im a g e
fo r m a t
is
not
s u p p o r te d
The ne survival probability for two flavor mixing is:
M a c in to s h P IC T im a g e fo rm a t
generatioRneqduetisres CC and ES/NC measurement Future expts (assum1in-3g%acti2v-e5o%sci1ll0a-t2io0n%s) 2-4%
Model-indep test for sterile n’s using measured oscillation parameters (p-p + KamLAND)
is n o t s u p p o rte d
Flavor eigenstates are a mixture of mass eigenstates
M a c in to s h
P IC T
im a g e
fo rm a t
is
n o t s u p p o rte d
States evolve with time or distance
– What is the radial temperature distribution of the Sun? – How do neutrino properties affect supernovae?
Nuclear Physics
Physics Program for Future Solar Neutrino Experiments (I)
Nuclear Physics
Neutrino Properties
• What We Don’t Know - Neutrino Properties
– Are neutrinos their own antiparticles? (Majorana n) – What is the absolute scale for neutrino mass? – Is the mass scale normal ordered or inverted hierarchy? – Are there sterile neutrinos? – What are the elements of the MNS mixing matrix? – Is CP / CPT violated in the neutrino sector?
• PrCVoaovrmtniihodpeueueastmrriesmiacdnesoptsnorafdlotriuhfivxofeeeesrpdsiermmnepcpsareelyeynicnbttiheCstahiePotenTntekhrtaoegeosfysnttmdefsrreyioipxslmeetienncmtdoghemeonafptuno4pgn.p4leeenxrt1loi0mf-1si9toGolanerV • SeFQasurseotcnlfuahorsrrrieLfteioiopqmvwr-uippt-inrreyseonomdvelair(tanrcgoggyonfdnuoneseleuuottltrrletsairritckribmunnmnudoioneytweouieoxolmtmefprndiesenntgrneoiienrmteoi10lxwefe/npnTqin-ttte1bsseh2)bumotifdrmufeeisnrctpoatbrsyheoevpbeaedrstt opfraonspyect
Mass-induced flavor oscillations
(with LMA as the favored solution)
Nuclear Physics
Neutrino Oscillations
If neutrinos have mass leptons can mix:
M a c in to s h P IC T im a g e fo rm a t
Precision test for CPT violation comparing
Macintosh PICT image format is not supported
and Macintosh PICT im age form at is not supported
Meoadseulr-edmeepnetnodf ethnet pc-rporsast-echtoec1%k fporrosvtideersilkennoewuletdrgineoosf q12 wtoitahllo≈w2a%seasrecnhsfiotirvCitPyT(9vi0o%latiConLa)t a scale of 10-20 GeV
• What We Don’t Know - Neutrino Astrophysics
– Is the Standard Solar Model correct? – What is the flux of solar neutrinos below 5 MeV?
• What is the flux of CNO neutrinos?
The Importance of Low-Energy Solar Neutrino Experiments
Thomas Bowles Los Alamos National Laboratory
Markov Symposium Institute for Nuclear Research
5/13/05
Sensitive to all flavors, but most sensitive to electron neutrinos
Nuclear Physics
What We Know
• Flux of 8B n’s has a large non-ne component • Survival probability Pee for En > 5 MeV is
essentially independent of En • Pee for n’s of lower energy (p-p) is larger • There is no significant (> 2s) D/N asymmetry
All observations are consistent with the following hypotheses:
is n o t s u p p o rte d
M a c in to s h P IC T im a g e fo rm a t
is n o t s u p p o rte d
Nuclear Physics
Flavor Content of the Solar 8B Neutrino Flux
Detecting Neutrinos in SNO
KamLAND observes a significant deficit of neutrinos and confirms solar neutrino LMA neutrino oscillation solution
Nuclear Physics
NeuKnow
CC Interaction
M a c in to s h P IC T im a g e fo r m a t
is n o t s u p p o r te d
Sensitive to electron neutrinos only
NC Interaction M a c i n t o s h P I C T im a g e fo r m a t is n o t s u p p o r te d
Can achieve ≈ 13% sensitivity (90% CL)
Nuclear Physics
Physics Program for Future Solar Neutrino Experiments (II)
• Use p-p neutrinos as “standard candle”
• 50 meV < mn < 2.8 eV (90% CL) – Lower limit from atmospheric neutrino results – Upper limit from tritium beta decay results
• Neutrinos account for at least as much mass in the Universe as the visible stars
Nuclear Physics
Standard Solar Model
Nuclear Physics
Comparison of measured rates and Standard Solar Model (After 30+ years of effort)
M a c in to s h P IC T im a g e fo rm a t
is n o t s u p p o rte d
Nuclear Physics
Reactor Neutrino Experiment
Photomultipliers
Terrestrial Neutrinos
K(NamOBLS A- NBDG)is/NaE1XPk=ton liquid scintillator detector t0h.a6t11ob±ser0v.0e8s5 (fsrtoamt) a num±be0r.0o4f1re(asycstot)rs in Japan at an average distance of 180 km
Expect sensitivity of 10-11 mB
Nuclear Physics
p-p Solar Neutrino Experiments: Physics Goals
Macintosh PICT image format is not supported
Equally sensitive to all flavours
ES Interaction
M a c in to s h P IC T im a g e fo rm a t
is n o t s u p p o rte d
• Directly observe the 99.99% of solar neutrinos that are below 5 MeV Direct test of solar models (p-p, 7Be, CNO)
• DMeetaesrumremiUnenencuterontfaitCianNrtiiOetsynin/eudtthireminseonslasprirononevuidotrefisnnaonmfliuimxxipensogrtmanat ttresixt: PresGo••efn1Cot.taN5hl%Oeispbot-fuoptrhnmseioneSlgaauirsnsp1u’ncs5-rrp’%eesunctteihora73gel1B5yif%ne%lisafivfrprosorC1trme0N1c0c0O%ito8shmiyeorCpnc86oNoBi%snnOivteicocytncilvee stage Witah• Pmproeosvdeiendlte-sintedset pofe1nin2di%teianltm8me%taanllnic1ei0try0%of the4%Sun
M a c in t o s h
P IC T
im a g e
fo r m a t
is
not
s u p p o r te d
The ne survival probability for two flavor mixing is:
M a c in to s h P IC T im a g e fo rm a t
generatioRneqduetisres CC and ES/NC measurement Future expts (assum1in-3g%acti2v-e5o%sci1ll0a-t2io0n%s) 2-4%
Model-indep test for sterile n’s using measured oscillation parameters (p-p + KamLAND)
is n o t s u p p o rte d
Flavor eigenstates are a mixture of mass eigenstates
M a c in to s h
P IC T
im a g e
fo rm a t
is
n o t s u p p o rte d
States evolve with time or distance
– What is the radial temperature distribution of the Sun? – How do neutrino properties affect supernovae?
Nuclear Physics
Physics Program for Future Solar Neutrino Experiments (I)
Nuclear Physics
Neutrino Properties
• What We Don’t Know - Neutrino Properties
– Are neutrinos their own antiparticles? (Majorana n) – What is the absolute scale for neutrino mass? – Is the mass scale normal ordered or inverted hierarchy? – Are there sterile neutrinos? – What are the elements of the MNS mixing matrix? – Is CP / CPT violated in the neutrino sector?
• PrCVoaovrmtniihodpeueueastmrriesmiacdnesoptsnorafdlotriuhfivxofeeeesrpdsiermmnepcpsareelyeynicnbttiheCstahiePotenTntekhrtaoegeosfysnttmdefsrreyioipxslmeetienncmtdoghemeonafptuno4pgn.p4leeenxrt1loi0mf-1si9toGolanerV • SeFQasurseotcnlfuahorsrrrieLfteioiopqmvwr-uippt-inrreyseonomdvelair(tanrcgoggyonfdnuoneseleuuottltrrletsairritckribmunnmnudoioneytweouieoxolmtmefprndiesenntgrneoiienrmteoi10lxwefe/npnTqin-ttte1bsseh2)bumotifdrmufeeisnrctpoatbrsyheoevpbeaedrstt opfraonspyect
Mass-induced flavor oscillations
(with LMA as the favored solution)
Nuclear Physics
Neutrino Oscillations
If neutrinos have mass leptons can mix:
M a c in to s h P IC T im a g e fo rm a t
Precision test for CPT violation comparing
Macintosh PICT image format is not supported
and Macintosh PICT im age form at is not supported
Meoadseulr-edmeepnetnodf ethnet pc-rporsast-echtoec1%k fporrosvtideersilkennoewuletdrgineoosf q12 wtoitahllo≈w2a%seasrecnhsfiotirvCitPyT(9vi0o%latiConLa)t a scale of 10-20 GeV
• What We Don’t Know - Neutrino Astrophysics
– Is the Standard Solar Model correct? – What is the flux of solar neutrinos below 5 MeV?
• What is the flux of CNO neutrinos?
The Importance of Low-Energy Solar Neutrino Experiments
Thomas Bowles Los Alamos National Laboratory
Markov Symposium Institute for Nuclear Research
5/13/05
Sensitive to all flavors, but most sensitive to electron neutrinos
Nuclear Physics
What We Know
• Flux of 8B n’s has a large non-ne component • Survival probability Pee for En > 5 MeV is
essentially independent of En • Pee for n’s of lower energy (p-p) is larger • There is no significant (> 2s) D/N asymmetry
All observations are consistent with the following hypotheses:
is n o t s u p p o rte d
M a c in to s h P IC T im a g e fo rm a t
is n o t s u p p o rte d
Nuclear Physics
Flavor Content of the Solar 8B Neutrino Flux
Detecting Neutrinos in SNO
KamLAND observes a significant deficit of neutrinos and confirms solar neutrino LMA neutrino oscillation solution
Nuclear Physics
NeuKnow
CC Interaction
M a c in to s h P IC T im a g e fo r m a t
is n o t s u p p o r te d
Sensitive to electron neutrinos only
NC Interaction M a c i n t o s h P I C T im a g e fo r m a t is n o t s u p p o r te d
Can achieve ≈ 13% sensitivity (90% CL)
Nuclear Physics
Physics Program for Future Solar Neutrino Experiments (II)
• Use p-p neutrinos as “standard candle”
• 50 meV < mn < 2.8 eV (90% CL) – Lower limit from atmospheric neutrino results – Upper limit from tritium beta decay results
• Neutrinos account for at least as much mass in the Universe as the visible stars
Nuclear Physics
Standard Solar Model
Nuclear Physics
Comparison of measured rates and Standard Solar Model (After 30+ years of effort)
M a c in to s h P IC T im a g e fo rm a t
is n o t s u p p o rte d
Nuclear Physics
Reactor Neutrino Experiment
Photomultipliers
Terrestrial Neutrinos
K(NamOBLS A- NBDG)is/NaE1XPk=ton liquid scintillator detector t0h.a6t11ob±ser0v.0e8s5 (fsrtoamt) a num±be0r.0o4f1re(asycstot)rs in Japan at an average distance of 180 km