the birth of the neutrino fiorini , varenna june 17, 2008 1. named neutrino by enrico fermi =>...
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The importance of being “Neutrino”
The birth of the neutrino
Ettore Fiorini , Varenna June 17, 20081
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Named Neutrino by Enrico Fermi => first properties of weak interactrions
ν e
n p
GF (Fermi constant)
Ettore Fiorini , Varenna June 17,2008
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More than 70 years of searches => parity violation, three flavours,lepton and flavor conservation (???)
Charged currents
Neutral currents
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Neutrino oscillations
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Ettore Fiorini , Varenna June 17, 20085
Solar neutrinos ( νe)
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Spectrum of solar neutrinos
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SNO and the New SNOLAB
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Geo-Neutrinos
• can we detect the antineutrinos produced bynatural radioactivity in the Earth?
radioactive decay of heavy elements(Uranium, Thorium) produces
antineutrinos
e ⇒
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Super-Kamiokande
νe ~ as predicted νµ deficit from below
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Atmospheric neutrinos
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Reactor Neutrinos
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2002:
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1051 m280 m
Double-CHOOZ (France) σινσιν22θ13 < 0.022θ13 < 0.022
σιν
σιν
22 2θ13
2θ13
0.030.03
Daya Bay (China)
DOUBLE CHOOZDOUBLE CHOOZ
Reactors (the future)
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Minos K2K
Simulated tau event:
Accelerators
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Two different hierarchy models
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CMB AnisotropyµK nK
WMAP
BOOMERanG DASI
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<mν> from Cosmology
mν = 0 eV mν = 1 eV
mν = 7 eV mν = 4 eV
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Tiny effect ->
Measurement (or limit ) on neutrino mass by single beta decay
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Katrin
3H => 3He + e- + νemν
< 2.2 eV => KATRIN < 0.2 eV
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The cryogenic or thermal detectors
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First ideas
1880 => Langley => resistive bolometers for infrrared from SUN
1905 => Curie et Laborde => calorimetric measurement of radioactivity
1927 => Ellis and Wuster => heat less then expected => the neutrino
1935 => Simon => sensitivity enhanced by lowering the temperature
1983 => T.Niinikoski =>observe pulses in resistors due to cosmic rays
=> McCammon et al (NASA-Wisconsin) Low temp. detectors for astrophysics and neutrino mass measurement1984 => Fiorini and Niinikoski Low temperature detectors for rare events
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Incidentparticle
absorber crystal
Thermal sensor
Excellent resolution <1 eV ~ 2eV @ 6 keV ~10 eV ~keV @ 2 MeV
VC
Q T =!
J/K )( v
v 1944 C 3
m
V
T
!=
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Non equilibrium and equilibrium detectors
-
- Various types of thermometers
=> a thermistor => a transition edge sensor (TES) => an Equilibrium Absorber weakly coupled to a heat bath superconducting tunnel junction (STJ) Cooper pair breaking => a magnetic thermometer . The temperature information is obtained from the change of a paramagnetic sensor placed in a small magnetic field
Caveat => possibility that the heat capacity of the thermometer be comparable or larger than the absorber one:
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Non equilibrium detectors
⇒ STJ Superconducting tunnel junctions⇒ SSG Superheated superconducting granules . The field does not enter
more in the granule. Often SQUID pickup Suggested for In solarneutrino detection. Considered for Dark Matter Experiments
=> Superfluid 3He and 4He detectors (rotons) . Also considered forSolar neutrinos
Comparison with conventional detectors:
=> Slow propagation of the vibration inside the absorber Kapitza resistence detector => heat sink (slow rise and decay times)
=> Possible localizazion of the event (TES)
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Macro and micro bolometers
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Energy resolution of a TeO2 crystal of 5x5x5 cm3 (~ 760 g )
: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 so far
Energy [keV]
210Po α line
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Orpheus 0.45 kg of granules 70 m.w.e for Dark Matter detection BernConsidered also for double beta decay (A.Morales)
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Q inner
Q outer
A
B
D
C
Rbias
I bias
SQUID array Phonon D
Rfeedback
Vqbias
Hybrid techniquesheat + ionization or heat + scintillation
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The scintillating bolometerProved for CaF2 being studied for TeO2
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8751 hours x mg (AgReO4)
MIBETA: Kurie plot of 6.2 ×106 Re ß-decay events (E > 700 eV)
10 crystals:
E0 = (2465.3 ± 0.5stat ± 1.6syst) eV
MANU2 (Genoa)metallic Rhenium
m ν< 26 eVNucl. Phys. B (Proc.Suppl.) 91 (2001) 293
MIBETA (Milano)AgReO4
mν < 15 eV
MARE (Milano, Como,Genoa, Trento, US, D)Phase I : mν < 2.5 eVm2
ν = (-112 ± 207 ± 90) eV2
Nucl. Instr. Meth. 125 (2004) 125
hep-ex/0509038
Microcalorimeters for Microcalorimeters for 187187Re ß-decayRe ß-decay
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A new fact in Material Science and Nuclear Physics=> Beta Environmenthal Fine Structure 187 Re => 187 Os + e- + ¯νe ΔE = 2.5 keV
The Genoa spectrum with metallic Rhenium
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The structure of BEFS has allowed to determine the P to S ratio of thebeta decay
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e- + 163 Ho => 163 Os + νe also for searches on neutrino mass
113 Cd => 113 I + e- + ¯ νe τ1/2 = (9+1) x 1015 y
e- + 123 Te => 123 Sb + νe τ1/2 > 1015 y
e- + 7 Be => 7 Li + νe => for solar neutrinos
e- + Ga => 71 Ge + νe => for solar neutrinos
First discovery of the decay 209 Bi => 204 Tl + α
Experiments with heavy ions
Other interesting results in nuclear physics obtatined withcryogenic detctors
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ProblemsProblems of of cryogeniccryogenic detectorsdetectors::The are slowThe are slow
and and totallytotally sensitive sensitivesurfacesurface contaminationcontamination
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What about the nature of the neutrino and its mass?
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→ →<= =>
Majorana=>1937
Neutrinoless double beta decay and Majorana neutrinos
RIGHT
LEFTν:
ν:
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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-
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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 been
calculated. The result is that this process occurs sufficiently rarely to allowan half-life of over 1017 years for a nucleus, even if its isobar of atomicnumber different by 2 were more stable by 20 times the electron mass
At the beginning At the beginning neutrinolessneutrinoless ββββ decay decay searched as the most powerful methodsearched as the most powerful methodto testto test conservation of lepton number. conservation of lepton number. Today, after discovery of Today, after discovery of neutrinoneutrino
oscillationsoscillations represents the best way to measure represents the best way to measure < <mmνν>>
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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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Predictions from neutrino oscillations
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Experimental approach
Direct ex-perimentsSource ≠ detectorSource = detector
(calorimetric)
Geochemical experiments82Se = > 82Kr, 96Zr = > 96Mo, 128Te = > 128Xe (non confirmed), 130Te = > 130Xe
Radiochemical experiments238U = > 238Pu (non confirmed)
e-
e-
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49
Nucleus T0n (y) 1 2 3 5 6 Faessler (Erratum)
48Ca >1.4x1022 2276Ge >1.9x1025 .47 .55 .41 .97 .84 .36 ±.0776Ge >1.6x1025 .51 .60 .44 1.1 .91 .40±.0876Ge 1.2x1025 .59 .69 .52 1.2 1.1 .46±.0982Se >2.1.x1023 2.2 2.9 1.8 2.8 3.7 1.9±2.0100Mo >5.8x1023 .97 2.7 1.1 11 1.1 ±.3116Cd >1.7x1023 2.4 3.5 1.4 2.7 2.3±.8128Te >7.7×1024 1.8 2.5 4.6 2.0 1.5±.6130Te >3x1024 .7 .85 .37 1.1 1.8 .48±.15136Xe >1.2x1024 2.9 2.0 .42 2.6 1.2±.5150Nd >1.2x1021 2.7 4.4 1.0 .84 8±4
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
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Claim of Evidence for 0νββ in 76Ge
Single-site events in detectors 2, 3, 4, 5 (56.6 kg-y).H.V. Klapdor-Kleingrothaus, Int. J. Mod. Phys. E17, 505 (2008)
<m> ~ 0.2 to 0.3 eV
Looks good to me…not to me (E.F.)
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Two new experiments NEMO III e CUORICINO
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Searches withthermal detectors
Cuoricino (Hall A)
CUORE (Hall A)
CUORE R&D (Hall C)
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Mass increase of bolometers
year
tota
l mas
s [k
g]
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DetectorsDetectors assemblingassembling
Operations carried outIn a clean room
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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 of TeO2Operation started in the beginning of 2003 => ~ 4 months
Background .18±.01 c /kev/ kg/ a T 1/2 0ν (130Te) > 3.1 x 1024 y <mν> .16 -.84 eV
Klapdor 0.1 – 0.9
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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)
Feruglio F. , Strumia A. , Vissani F. hep-ph/0201291
Arnaboldi et al., submitted to PRL, hep-ex/0501034(2005).
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Experiment Nucleus Detector
NEMO III 100
Mo et al 10 kg of enrich. Isotopes -tracking
Cuoricino 130Te + etc. 40 kg of TeO 2 bolometers (nat)
CUORE 130
Te + etc. 750 kg of TeO 2 bolometers (nat)
EXO 136
Xe 200kg - 1 t Xe TPC
GERDA 76
Ge 30-40 kg - 1t Ge diodes in LN
Majorana 76
Ge
180 kg - 1t Ge diodes
MOON 100Mo nat.Mo sheets in plastic sc.
DCBA 150
Nd
20 kg Nd -tracking
CAMEO 116
Cd
1 t CdWO 4 in liquid scintillator
COBRA 116
Cd , 130
Te
10 kg of CdTe semiconductors
Candles 48Ca Tons of CaF 2 in liquid scintillators
GSO 116
Cd
2 t Gd 2SiO5:Ce scintill.in liquid sc.
Xe 136
Xe
1.56 Xenon in liquid scintillator.
Xmass 136
Xe
1 t of liquid Xe
MOON
CUORE
GERDA
EXO
CUORICINO
22PP1/21/2
44DD3/23/222SS1/21/2
493 nm493 nm650 nm650 nm
metastablemetastable 47s47s
Experimental situation
58
CUORE
SNO++
MOON
NEMO - SuperNEMO
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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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Compound Isotopic abundance Transition energy
48CaF2 .0187 % 4272keV76Ge 7.44 " 2038.7 "
100MoPbO4 9.63 " 3034 "
116CdWO4 7.49 " 2804 "130TeO2 34 " 2528 "
150NdF3150NdGaO3
5.64 " 3368“
Other possible candidates for Other possible candidates for neutrinolessneutrinoless DBD DBD
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Neutrino oscillations exist => Δm ν 2 ≠ 0
Future experiments will enable to investigate in details the parameters of this processDetermination of the absolute value of <mν > becomes imperativeTheory indicates <mν > from a from few to a few tens of meV.The study of Cosmic Microwave Background determines the sum of neutrino masseswith high precision. How much model dependent?Single beta decay constraints directly <m ν> but still far from predictionsFuture experiment on neutrinoless double beta decay could determine <mn > at thelevel predicted by neutrino oscillations under the inverse hierarchy hypothesis, andascertain if neutrino is a Majorana particleThe present claim for this phenomenon indicating <mν > ~0.44 eV is not confirmed byCUORICINOThe most advanced and sometime not yet tested nuclear physics techniques are beingstudied for future DBD experimentDeterminaion of neutrino mass involves already nuclear and sub nuclear physics. Itspeculiar multidisciplinarity involves fundamental problems in astroparticle physics,radioactivity’, materials, geochronology ecc.Very stimulating for young people
CONCLUSIONS
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From now on one should discuss seriously all side ofthe problem. Therefore , dear radioactive people , doinvestigate and judge.
Unfortunately I cannot be personally inTubingen since my presence is absolutelyindispensable here for a ball that will take place herein the night between December 6 and 7.
Your devoted servantWolfang Pauli
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From the letter of From the letter of WolfangWolfang PauliPauli of December 1, 1930 of December 1, 1930