Neutrino Oscillations and Astroparticle Physics (1)
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Neutrino Oscillations and Astroparticle Physics (1) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS)
Pisa, 6 May 2002
Introduction to Astroparticle Physics Neutrinos - Number - Dirac and Majorana Neutrinos - Mass Measurements - Double Beta Decay - Mixing
Neutrino Oscillations
Cosmology
Dark Matter
High Energy Astronomy
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What is Astroparticle physics ?
Particle Physics
Astronomy
Astrophysics and cosmology
PARTICLE
ASTROPHYSICS
Particle Astrophysics/Nuclear Astrophysics
Use input from Particle Physics to explain universe: Big Bang, Dark Matter, ….
Use techniques from Particle Physics to advance Astronomy
Use particles from outer space to advance particle physics
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Story of the Universe
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Make-up of Universe
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Dark MatterEvidence : Need to hold together Galaxy Clusters Explain Galaxy Rotation velocities
Astronomy object candidates : Brown Dwarfs (stars mass <0.1 Msun no fusion) - some but not enough White Dwarfs ( final states of small stars) - some but not enough Neutron Stars/Black Holes ( final states of big stars.) - expected to be rarer than white dwarfs Gas clouds - 75% visible matter in the universe, but observable
Particle Physics candidates: Neutrinos - Evidence for mass from oscillation, not enough for all Axions - Difficult to detect …. Neutralinos - Particle Physicist Favourite !
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charged particles protons ions electronsneutral particles photons neutrinos
at ground level :~ 1/sec/m²
Primary cosmic raysproduce showers in high atmosphere
Primary: p 80 %, 9 %, n 8 % e 2 %, heavy nuclei 1 % 0.1 %, 0.1 % ?
Secondary at ground level: 68 % 30 % p, n, ... 2 %100 years after discovery by Hess origin still uncertain
Cosmic Rays
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Particle Acceleration
R 1015km, B 1010T E 1000 TeV
R 10 km, B 10 T E 10 TeV
Large Hadron Collider
Tycho SuperNova Remnant
E BR
( NB. E Z Pb/Fe higher energy)
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Energy of particules accelerated
Dia
met
er o
f co
llid
er
Cyclotron Berkeley 1937
Saturne, Saclay, 1964
Particle Physics Particle Astrophysics
LHC CERN, Geneva, 2005
Terrestrial Accelerators Cosmic Accelerators
Active Galactic Nuclei
Binary Systems
SuperNova Remnant
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Ultra High Energy from Cosmic Rays
1 102 104 106 108 1010 1012 Energy GeV
1 102 104 106 108 1010 1012 Energy GeV
cro
ss-s
ecti
on (
mb
)
par
ticl
e fl
ux
/m2 /
st/s
ec/G
eV
From laboratory accelerators From cosmic accelerators
FNAL LHC FNAL LHC
Flux of cosmic ray particles arriving on Earth
Particle cross-sections measured in accelerator experiments
Ultra High Energy Particles arrive from space for free: make use of them
Colliders Colliders
Fixed target beamlines
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absorption cut-off mean free path -rays: + 2.7k >1014eV 10 Mpc
proton: p + 2.7k 0 + X >5.1019eV 50 Mpc
nuclei: photo-disintegration >5.1019eV 50 Mpcneutrinos: + 1.95K Z+X >4.1022eV (40 Gpc)
magnetic deflection
(rad)= L(kpc) Z B(G)/E(EeV) Galaxy B=2G, Z=1, L=1kpc -> =12deg at 1019eV
Photons absorbed on dust and radiation
Protons deviated by magnetic fields
Neutrinos direct
Multi-Messanger Astronomy
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Neutrino Mass in the Universe
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Neutrino History
1931 - Predicted by Pauli
1934 - Fermi develops a theory of radioactive decays and invents name neutrino
1959 - Discovery of neutrino (e) is announced by Cowan and Reines
1962 - Experiments at Brookhaven and CERN discover the second neutrino:
1968 - First evidence that solar neutrino rate half expectation: "solar neutrino problem”
1978 - Tau particle is discovered at SLAC by Perl et al.: infer third neutrino
1985 - First reports of a non-zero neutrino mass (still not confirmed)
1987 - Kamiokande and IMB detect bursts of neutrinos from Supernova 1987A
1988 - Kamiokande reports only 60% of the expected number of atmospheric
1989 - Experiments at LEP determine three neutrinos from Z line width
1997 - Super-Kamiokande see clear deficits of atmospheric and solar e
1998 - The Super-Kamiokande announces evidence of non-zero neutrino mass
2000 - DONUT experiment claims first observation of tau neutrinos
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First observation of Neutrino
Reines and Cowan 1959: Target made of 400 l water and cadmium chloride near reactor. The anti-neutrino coming from the nuclear reactor interacts with aproton of the target matter, giving a positron and a neutron. The positron annihilates with an electron of the surrounding material, giving two simultaneous photons and the neutron slows down until it iseventually captured by a cadmium nucleus, implying the emission of photons some 15 microseconds after those of the positron annihilation. All those photons are detected and the 15 microseconds identify theneutrino interaction.
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Three Generations of Particles Mass(Mev/c2)
At present only limits of absolute masses of neutrinosOscillations give neutrino mass differences
s
ue
d
e
c
t
b
106
104
102
1
102
104
106
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Discovery of (?)
DONUT experiment, FNAL
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Discovery of (?)
4
eventsidentified
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Number of Neutrino Families
Data
From Big Bang Nucleosynthesis
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Number of Neutrino Families From Big Bang Nucleosynthesis
Fraction 4He
Fraction Li
Lifetime (s) Reference 918 ± 14 [Chr72] 903 ± 13 [Kos86] 891 ± 9 [Spi88] 876 ± 21 [Las88] 877 ± 10 [Pau89] 888 ± 3 [Mam93] 878 ± 30 [Kos89] 894 ± 5 [Byr90]888.4 ± 4.2 [Nes92]882.6 ± 2.7 [Mam89]887.0 ± 2.0 [PDG94]
Dependence on Neutron lifetime
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Number of Neutrino FamiliesMeasurements from LEP of width of Z resonance
N = 2.994±0.012
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Neutrino Mass MeasurementsDirect mass measurements - Time-of-flight measurements from distant objects - Kinematics of Weak Decays
Indirect searches ( effects which only exist if M( ) 0 )
- Neutrino Oscillations - Neutrinoless Double Beta Decay
even
ts
energy
XY
M()=0M()0
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Dirac and Majorana Neutrinos
( See Akhmedov ‘ Neutrino physics ’ : hep-ph/0001264 )
For massive fermion, mass term in Lagrangian:
Mass term couples left and right-handed components:
Dirac Neutrino: left and right-handed fields completely independentMajorana Neutrino : left and right-handed fields charge conjugates
then:
so:
Majorana neutrino is its own anti-particle
: Majorana field is self charge-conjugate
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Dirac and Majorana masses
General neutrino mass term in Lagrangian:
where:
Mass matrices : Dirac mD, Majorana mL, mR
n species of neutrino: n n complex matrices
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Supernova 1987a in Large Magellenic Cloud L = 50 kpc (150 light years )
p e ne
e+ e e + e, ,
Neutrino Mass from Time-of-flight
M(e ) < 23 eV/c2
t = 0 unknownuse arrival time as function of energy
time (sec) time (sec)
energy (MeV)
eve
nts
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Limits on M( )
Measured in decays at LEPe+e + n (n=3, 5, 6)
contours are limits when E = 0
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Limits on M( )
In tau rest frame energy of hadronic system h:
E*h =
m2 + mh
2 m2
2 m
Total decays 2939 : 2 + 52 : 3 2+
3 : 3 2+ 0
only events with high mh
contribute to M( ) limitM( ) < 18.2 MeV/c2 (95% CL)
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Limits on M( )
M( ) < 170 keV/c2 (95% CL)
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Limits on M(e )
Detailed study of end-point of spectrum: many experiments
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Limits on M(e )
Mainz spectrometer
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Limits on M(e )
End-point spectra
Troitsk experiment Mainz experiment
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Limits on M(e )
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0
Double Beta DecayA(Z,N) A(Z+2, N2)+2e
(neutrino-less)
A(Z,N) A(Z+2, N2)+2e+2e
Only possible M() 0Majorana neutrino
2
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Must be energetically allowedand single beta decay suppressed
Only a few possible double beta isotopes
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Example: 100Mo in MOON detector
100Mo 100 Ru + 2 e (+ 2 e )
Both: Double beta decay:
Solar neutrino: 100Mo + e 100Mo 100 Tc + e 100 Ru + e
Mo(42,48) Ru(44, 46)
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Physics beyond Standard Model in 0
Right-Handed Currents
Majoron production
Supersymmetry
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NEMO 3 (100Mo)At Modane laboratory in Frejus tunnel
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Heidelberg-Moscow (76Ge)At Gran Sasso laboratory
signal of 2 expected 0
Half-life T½2 = 1.55±0.17 1021 years T½
0 > 3.1 1025 years (90% CL)
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Summary of Double Beta Decay Results
Limits on Majorana neutrino mass
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Latest News
August 2001 limit:T½
0 > 3.1 1025 years (90% CL) M < 0.3 eV /c2
January 2002 evidence:T½
0 = (0.8-18.3) 1025 years (95%CL) 1.5 1025 years: best value M = 0.11-0.56 eV /c2 (95% CL) = 0.39 eV /c2: best value
- same data, not all same people…..
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Summary of Particle Data Group 2001
M( e ) < 3 eV /c2
M( ) < 190 keV/c2
M( ) < 18.2 MeV/c2
Majorana mass M(e ) < 0.24 eV /c2
( dependent on Nuclear Matrix Element)
Number of light : 2.994 0.012
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Possible Neutrino Mass Splitting
Zero of mass scale ?
M(e) < 3 eV ?
0
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Neutrino MixingAnalogy with quarks
For massive particles: flavour eigenstates can be different from mass eigenstates
=
d
s
b
d
s
b
Vud Vus Vub
Vcd Vcs Vcb
Vtd Vts Vtb
leptons quarks
U : leptonic mixing matrixV : quark mixing matrix, ( CKM matrix ) Standard Model, U and V unitary 3 3 complex matrices: Uk
* Uk =
=
e
Ue1 Ue2 Ue3
U1 U2 U3
U1 U2 U3
1
2
3
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W decaysleptons quarks
W q q W l l
W e 1 Ue1 2 e 2 Ue2 2
e 2 Ue3 2
1 U1 2 2 U2 2
3 U3 2
1 U1 2 2 U2 2
3 U3 2
W u d Vud 2 u s Vus 2
u b Vub 2
c d Vcd 2 c s Vcs 2
c b Vcb 2
( t X m(t) > m(W) )
Unitarity: Ue1 2 + Ue2 2 + Ue3 2 = 1
etc.
Vud 2 + Vus 2 + Vub 2 = 1
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Numerical Values
0.97 0.22 0.003
0.22 1.0 0.04
0.006 0.04 1.0
Vud Vus Vub
Vcd Vcs Vcb
Vtd Vts Vtb
Ue1 Ue2 Ue3
U1 U2 U3
U1 U2 U3
?
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Possibilities for Leptonic Mixing
Ue1 Ue2 Ue3
U1 U2 U3
U1 U2 U3
0.97 0.22 0.003
0.22 1.0 0.04
0.006 0.04 1.0
1 0 0
0 1 0
0 0 1
1/2 1/2 0
1/2 1/2 1/2
1/2 1/2 1/2
No mixing like quarks bi-maximal mixing
If Ue3 = 0 no CP violation ( like Vub = 0 for quarks)
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CP Violation in Neutrino Sector
Ue1 Ue2 Ue3
U1 U2 U3
U1 U2 U3 If Ue3 = 0 no CP violation ( like Vub = 0 for quarks)
CP conservation:
Same parameterisation as quark sector: