double beta decay and majorana neutrinos · 23 11 modules, 4 detector each, crystal dimension 5x5x5...
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Double beta decay and Majorana neutrinos
Presently an essential problem in neutrino andin astroparticle physiss
→ →<= => Majorana =>1937
Ettore Fiorini, Venice March 8, 2007
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The most sensitive way to investigate the Dirac or Majorana nature of theneutrino is neutrinoless double beta decay (DBD)This very rare process was sugested in general form by Maria Goepper Mayerjust one year after the Fermi theory of beta decay. Also Bruno Pontecorvo wasdeeply involved.
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Double Beta –Disintegration
M.Goeppert-Mayer, The John Hopkins University(Received May, 20 , 1935)
From the Fermi theory of β− disintegration the probability ofsimultameous emission of two electrons (and two neutrinos) has beencalculated. The result is that this process occurs sufficiently rarely toallow an half-life of over 1017 years for a nucleus, even if its isobar ofatomic number different by 2 were more stable by 20 times the electronmass
Double beta decay was at the beginning searched In the Double beta decay was at the beginning searched In the neutrinolessneutrinolesschannel as a powerful way to search for channel as a powerful way to search for lepton number nonlepton number nonconservationconservation. Presently it is also considered as the most powerful. Presently it is also considered as the most powerfulway to investigate the value of the way to investigate the value of the massmass of a of a MajoranaMajorana neutrino neutrino
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1. (A,Z) => (A,Z+2) + 2 e- + 2 νe¯2. (A,Z) => (A,Z+2) + 2 e- + χ ( …2,3 χ)3. (A,Z) => (A,Z+2) + 2 e-
Process 1 has been detected in ten nucleiProcess2 and 3. violate the lepton numberProcess 3, normally called neutrinoless DBD, would be revealed bythe presence of a peak in the sum of the electron energies => <mν>≠ 0
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u e -d
de -
W
u
νe
νe
2ν - ββ decay
W
0ν - ββ decay
e -
e -
d
du
u
WW
eνe
ν
Neutrinoless ββ decay
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1/τ = G(Q,Z) |Mnucl|2 <mν>2
rate of DDB-0ν Phase space Nuclear matrix elements
EffectiveMajorana neutrino mass
The rate of neutrinoless DBD strongly depends on theevaluation of the nuclear matrix elements, quite
uncertain so far
Need to search for neutrinoless DBD in various nucleiA pick could be due to some unforeseen background peak
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Possible schemes for neutrino masses
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New calculations by.S.Pascoli and S.T.Petkov
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Experimental approaches
Direct experiments
Source ≠ detectorSource = detector(calorimetric)
Geochemical experimentsi82Se = > 82Kr, 96Zr = > 96Mo (?) , 128Te = > 128Xe (non confirmed), 130Te = > 130Te
Radiochemical experiments238U = > 238Pu (non confirmed)
e-
e-
e-
e-
source
detector
detector
Source ≠ Detector
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Incidentparticle
absorber crystal
heat bath
Thermal sensor
Cryogenic detectors
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2T
VCk E !="
ΔΕ @ 5 keV ~100 mk ~ 1 mg <1 eV
~ 3 eV @ 2 MeV ~10 mk ~ 1 kg <10 eV ~
keV
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Resolution of the 5x5x5 cm3(~ 760 g ) crystals
:0.8 keV FWHM @ 46 keV1.4 keV FWHM @ 0.351 MeV2.1 keV FWHM @ 0.911 MeV2.6 keV FWHM @ 2.615 MeV3.2 keV FWHM @ 5.407 MeV
(the best α spectrometer everrealized)
Energy [keV]
Cou
nts
210Po α line
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1.1 -2.9>1.2x1024scintillator6924768.9DAMA136Xe
3 - ?>1.2x1021tracking9133675.6Irvine150Nd
.16-.82.>2x1024bolometric252933.8Cuoricino130Te
.1-4>7.7 × 1024geochem252934Bernatovitz128Te
1.7 - ?>1.7x1023scintillator8330347.5Solotvina116Cd
.7-2.8>4.6x1023tracking95-9930349.6NEMO 3100Mo
1.8-4.9>1.x1023tracking9729959.2NEMO 382Se
.441.2x1025ionization8720397.8Klapdor et al76Ge
.14 – 1.2>1.6x1025Ionization8720397.8IGEX76Ge
.12 - 1>1.9x1025ionization8720397.8Heidelberg-Moscow
76Ge
7-45>1.4x1022scintillator42710.19Elegant IV48Ca
<mν)Τ0ν (y)TechniqueEnrQββ%ExperimentNucleus
Present experimental situationPresent experimental situation
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HM collaboration subset (KDHK):HM collaboration subset (KDHK):claim of evidence of 0claim of evidence of 0νν-DBD-DBD
In December 2001, 4 authors (KDHK) of the HM collaboration announce the discovery of neutrinoless DBD
τ1/20ν (y) = (0.8 – 18.3) × 1025 y (1 × 1025 y b.v.)
〈Mββ〉 = 0.05 - 0.84 eV (95% c.l.)
54.98 kg•y 2.2 σ
2001
71.7 kg•y 4 σ
2004
skepticism in DBD community in 2001 better results in 2004
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Two new experiments NEMO III and CUORICINO
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100Mo 6.914 kg Qββ = 3034 keV
82Se 0.932 kg Qββ = 2995 keV
116Cd 405 g Qββ = 2805 keV
96Zr 9.4 g Qββ = 3350 keV
150Nd 37.0 g Qββ = 3367 keV
Cu 621 g
48Ca 7.0 g Qββ = 4272 keV
natTe 491 g
130Te 454 g Qββ = 2529 keV
ββ2ν measurement
External bkg measurement
ββ0ν search
ββββ decay isotopes in NEMO-3 detector decay isotopes in NEMO-3 detector
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0ν analysis
100Mo ⇒ τ1/20ν (y) > 4.6 × 1023 〈Mββ〉 < 0.7 – 2.8 eV (90% c.l.)
82Se ⇒ τ1/20ν (y) > 1.0 × 1023 〈Mββ〉 < 1.7 – 4.9 eV (90% c.l.)
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CUORICINO
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11 modules, 4 detector each,crystal dimension 5x5x5 cm3
crystal mass 790 g4 x 11 x 0.79 = 34.76 kg of TeO2
2 modules, 9 detector each,crystal dimension 3x3x6 cm3
crystal mass 330 g9 x 2 x 0.33 = 5.94 kg of TeO2
Search for the 2β|oν in 130Te (Q=2529 keV) and other rare events
At Hall A in the Laboratori Nazionali del Gran Sasso (LNGS)
18 crystals 3x3x6 cm3 + 44 crystals 5x5x5 cm3 = 40.7 kg ofTeO2Operation started in the beginning of 2003 => ~ 4 months
Background .18±.01 c /kev/ kg/ a
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Present CUORICINO result (new)Present CUORICINO result (new)
60Co pile-up peak
130Te DBD Q-value
anticoincidence spectrum 208Tl line
Energy [keV]
detail
DBD
MT = 5.87 (kg 130Te) x y
b = 0.18 ± 0.02 c/keV/kg/y
(Jul 2005)
8.35 kg year of 130Te
<m0ν> < .16 - .9 eV =>
τ >3 x 1024 (90 % c.l.)
Klapdor et al m0ν < .1- .9 eV
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Cosmological disfavoured region (WMAP)
Direct hierarchyΔm2
12= Δm2
sol
Inverse hierarchyΔm2
12= Δm2atm
“quasi” degeneracym1≈ m2 ≈ m3
With the same matrix elements the Cuoricino limit is 0.53 eV
Present Cuoricino region
Possible evidence(best value 0.39 eV)
H.V. Klapdor-Kleingrothaus et al., Nucl.Instrum.andMeth. ,522, 367 (2004).
Feruglio F. , Strumia A. , Vissani F. hep-ph/0201291
Arnaboldi et al., submitted to PRL, hep-ex/0501034(2005).
DBD and Neutrino Masses
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27Scintillation33675.6150NdSNOLAB+Ionization28057.5115CdCOBRA
65-?Scintillation1x1026200-173022160GdGSO50-94Scintillation3x1027-4271.1948CaCARVEL29-54Scintillation3x1027.35-4271.1948CaCandles16-22Tracking1x10268033675.6150NdDCBA-213-48Tracking1.7x10273.88530349.6100MoMoon-312-31Tracking1.3x1028.556524768.9136XeEXO
54-167Tracking2102619029958.782SeSupernemo13-42Ionization1x1028.49020397.876GeGENIUS21-67Ionization4x1027.69020397.876GeMajorana29-94Ionization2x10273.859020397.876GeGERDA9-57Bolometric1.8x10273.590253334130TeCUORE
<m>TechT (year)Bc/y
% EQββ%Name
Next generation experiments
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Ionization
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COBRAIonization
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C0BRA
Use large amount of CdZnTe Semiconductor Detectors
Array of 1cm3
CdTe detectors
K. Zuber, Phys. Lett. B 519,1 (2001)
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• 0n: 1000 eventsper
• year with 1%natural
• Nd-loaded liquid• scintillator in
SNO++
Nd dissolved in SNO => tons of material;
maximum likelihood statistical test of the shape to extract0ν and 2ν components…~240 units of Δχ2 significance after only 1 year!
simulation:one year of data
by Alex Wright
Scintillation
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Scintillation
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Tracking SUPERNEMO
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Tracking
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■ conceptconcept: scale Gotthard experiment addingBa taggingBa tagging to suppress background (136Xe136Ba+2e)
■ single Ba detected by optical spectroscopy■ two options with 63% enriched Xe
►High pressure Xe TPCHigh pressure Xe TPC►LXe TPC + scintillationLXe TPC + scintillation
■ calorimetry + trackingcalorimetry + tracking■ expected bkg only by -2
►energy resolution E = 2%
Present R&DPresent R&D■ Ba+ spectroscopy in HP Xe / Ba+ extr.■ energy resolution in LXe (ion.+scint.)■ Prototype scale:► 200 kg enriched L136Xe without tagging► all EXO functionality except Ba id► operate in WIPP for ~two years■Protorype goals:►Test all technical aspects of EXO
(except Ba id)►Measure 2ν mode►Set decent limit for 0ν mode
(probe Heidelberg- Moscow)
22PP1/21/2
44DD3/23/222SS1/21/2
493 nm493 nm650 nm650 nm
metastable metastable 47s47s
LXe TPCLXe TPC
EXOEXO
Full scale experiment at WIPP orFull scale experiment at WIPP orSNOLABSNOLAB■10 t10 t (for LXe ⇒ 3 m3)
►b = 4×10-3 c/keV/ton/y►1/21/2 1.31.3××10102828 y y in 5 years►⏐⏐mm
⏐⏐ 0.013 0.013 ÷÷ 0.037 eV 0.037 eV
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CUORE CUORE expectedexpected sensitivitysensitivity
disfavoured by cosmology
11-576.5 _ 10 26510-3
19-1002.1 _ 10 26510-2
<m!> [meV]T1/2 [y]"
[keV]b (counts/keV/kg/y)
11-576.5 _ 10 26510-3
19-1002.1 _ 10 26510-2
<m!> [meV]T1/2 [y]"
[keV]b (counts/keV/kg/y)
Strumia A. and Vissani F. hep-ph/0503246
In 5 years:
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3368“5.64 " 150NdF3150NdGaO3
2528 "34 "130TeO2
2804 "7.49 "116CdWO4
3034 "9.63 "100MoPbO4
2038.7 "7.44 "76Ge
4272 keV.0187 %48CaF2
Transition energyIsotopic abundanceCompound
130Te has high transition energy and 34% isotopic abundance => enrichmentnon needed and/or very cheap. Any future extensions are possiblePerformance of CUORE, amply tested with CUORICINO
Other possible candidates for neutrinoless DBD Other possible candidates for neutrinoless DBD
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How deep should we go?
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Total Muon Flux v.s. Depth Relative to Flat Overburden(cm-2 s-1)
Depth (km.w.e) Relative to Flat Overburden
Tota
l
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Neutron Flux at Underground Sites
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eg. Study for 60 kg Majorana Module
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Neutrino oscillations ⇒ Δm2 ≠0 ⇒ <mν> finite for at leaqst one neutrino
Neutrinoless double beta decay would indicate if neutrino is a lepton violatingMajorana particle and would allow in this case to determine <mn> and thehierachy of oscillations.
This process has been indicated by an experiment (Klapdor) with a value of~0.44 eV but has not yet confirmed
Future experiments on neutrinoless double beta decay will allow to reach thesensitivity predicted by oscillations
The multidisciplinarity of searches on double beta decay involves nuclear ande subnuclear physics, astrophysics , radioactivity, material science,geochronology etc. It could help in explaining the particle-antiparticleasymmetry of the Universe
CONCLUSIONS