neutrino oscillations and physics beyond the smschoning/... · a.schöning 15 particle physics ws...
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A.Schöning 1 Particle Physics WS 16/17
Neutrino Oscillations andPhysics Beyond the SM
● Neutrino● PMNS Matrix● Maiorana Neutrinos● (Supersymmetry)
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A.Schöning 2 Particle Physics WS 16/17
Solar Neutrino Reactions
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A.Schöning 3 Particle Physics WS 16/17
Solar Neutrino Experiments
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A.Schöning 4 Particle Physics WS 16/17
KamiokandeBig Water Cerenkov Detector
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A.Schöning 5 Particle Physics WS 16/17
Solar Neutrino Deficits
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A.Schöning 6 Particle Physics WS 16/17
Reactor Neutrino Oscillations
KAMLAND: anti electron neutrinos
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A.Schöning 7 Particle Physics WS 16/17
Neutrino Oscillations● “Classical” SM: v
e, v
mu, v
tau are massless → no mixing
● Massive neutrinos:
∣ν(t ) ⟩ =∣ν(0)⟩ e−i (Et−kz )oscillation frequency depends on neutrino mass∣ν(t) ⟩ ≈∣ν(0) ⟩ e
−im2 t2k e−i (kt−kz )
common factor for all neutrinosdepends on neutrino species
● Two generation mixing
P (νe→νe)(t )≈ 1− sin2(2Θ) sin2(Δm12
2 t
4 k)
P (νe→νμ)(t) ≈ sin2(2Θ) sin2(
Δm122 t
4 k)
sin2Δm12
2 t
4 k= sin2(π L /L0)
Θ = mixing angle
Δm12
2 = mass2 difference
L0= 2.47p
Δm122
eV 2mMeV
sun v: ~MeVatmospheric v: ~GeVreactor v: ~ 100 keV
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A.Schöning 8 Particle Physics WS 16/17
Solar Neutrino Mixing
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A.Schöning 9 Particle Physics WS 16/17
Cosmic Showers
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A.Schöning 10 Particle Physics WS 16/17
Super Kamiokande
Cerenkov Images:
electron muon
photomultipliersin water tank
νe → e W+ ν
μ → μ W+
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A.Schöning 11 Particle Physics WS 16/17
Super-Kamiokande Atmospheric Neutrinos
deficit of upgoing muon neutrinos
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A.Schöning 12 Particle Physics WS 16/17
“Atmospheric Mixing”
MINOS and K2K are muon-neutrino-beam experiments
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A.Schöning 13 Particle Physics WS 16/17
PMNS Matrix and Hierarchy
Θ ~45°
Θ ~35°
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A.Schöning 14 Particle Physics WS 16/17
atmosphericneutrinos
solar neutrinos
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A.Schöning 15 Particle Physics WS 16/17
Beyond the SM
Observations not explained by (extended) SM dark matter
Problems of the SM● generations of fermions● fermion masses and mixing● neutrinos (Maiorana or Dirac) and generation of masses● Hierarchy problem
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A.Schöning 16 Particle Physics WS 16/17
The SM Hierarchy (Fine Tuning) Problem● Fermion-Higgs couplings do not decouple in the SM
→ leading to large negative radiative contributions to Higgs mass● Similar contributions from Higgs self-coupling, but positive
∝g2
mtM W
→ In SUSY the quadratic divergences from fermion loops are compensated by additional scalar fermions. Only usual logarithmic divergences remain.
Higgs mass then given by
MHiggs
/MPlanck
= 10-17 is considered to be unnatural → fine tuning problem
scalar loop fermion
δM H2
= M H ,bare2
+ δM H2
M Hf2 =
∣g f2∣
162 [−22 6m f2 log /m f ]M Hs
2 =∣s
2∣162 [ 2 2ms
2 log /ms ]
note factor 2
H H
H
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A.Schöning 17 Particle Physics WS 16/17
SupersymmetryJ=1/2 J=1 J=0 J=1/2 J=1/2 J=0
scalar particles fermions
Gauginos are dark matter candidates
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A.Schöning 18 Particle Physics WS 16/17
Unification of Gauge Couplings
SMMSSM
unification point
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A.Schöning 19 Particle Physics WS 16/17