neutrinos – ghost particles of the universe
DESCRIPTION
Neutrinos – Ghost Particles of the Universe. Neutrinos Ghost Particles of the Universe. Georg G. Raffelt Max-Planck-Institut f ür Physik, München, Germany. Periodic System of Elementary Particles. Quarks. Leptons. Charge + 2/3 . Charge - 1/3 . Charge - 1 . - PowerPoint PPT PresentationTRANSCRIPT
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrinos – Ghost Particles of the UniverseNeutrinos
Ghost Particles of the Universe
Georg G. RaffeltMax-Planck-Institut für Physik, München, Germany
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutron
ProtonGravitation (Gravitons?)
Weak Interaction (W and Z Bosons)
Periodic System of Elementary Particles
Electromagnetic Interaction (Photon)
Strong Interaction (8 Gluons)
Down
Strange
Bottom
Electron
Muon
Tau
e-Neutrino
m-Neutrino
t-Neutrino nt
nm
nee
m
t
d
s
b
1st Family
2nd Family
3rd Family
Up
Charm
Top
u
c
t
Quarks Leptons
Charge -1/3
Down
Charge -1
Electron
Charge 0
e-Neutrino need
Charge +2/3
Up u
Where do Neutrinos Appear in Nature?
Nuclear Reactors
Particle Accelerators
Earth Atmosphere(Cosmic Rays)
Earth Crust(Natural Radioactivity)
AstrophysicalAccelerators Soon ?
Sun
Supernovae(Stellar Collapse) SN 1987A
Cosmic Big Bang (Today 330 n/cm3) Indirect Evidence
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Pauli’s Explanation of the Beta Decay Spectrum (1930)
Niels Bohr:Energy notconserved inthe quantumdomain?“Neutron”
(1930)Wolfgang Pauli(1900–1958)Nobel Prize 1945
“Neutron”(1930)
“Neutrino”(E. Fermi)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrinos from the Sun
Reaction-chains
Energy26.7 MeV
Helium
Solar radiation: 98 % light 2 % neutrinosAt Earth 66 billion neutrinos/cm2 sec
Hans Bethe (1906-2005, Nobel prize 1967)Thermonuclear reaction chains (1938)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Sun Glasses for Neutrinos?
8.3 light minutes
Several light years of lead needed to shield solar neutrinos
Bethe & Peierls 1934: … this evidently means that one will never be able to observe a neutrino.
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
First Detection (1954 – 1956)
Fred Reines(1918 – 1998)Nobel prize 1995
Clyde Cowan(1919 – 1974)
Detector prototype
Anti-Electron Neutrinosfrom Hanford Nuclear Reactor
3 Gammasin coincidence𝝂𝐞 p
n Cd
e+¿ ¿ e−
g
g
g
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
First Measurement of Solar Neutrinos
600 tons ofPerchloroethylene
Homestake solar neutrino observatory (1967–2002)
Inverse beta decayof chlorine
Cherenkov Effect
Water
Elastic scattering or CC reaction
NeutrinoLight
Light
Cherenkov Ring
Electron or Muon(Charged Particle)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Super-Kamiokande Neutrino Detector (Since 1996)
42 m
39.3 m
Super-Kamiokande: Sun in the Light of Neutrinos
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrino Flavor Oscillations
Bruno Pontecorvo(1913–1993)
Invented nu oscillations
Two-flavor mixing
Each mass eigenstate propagates as with Phase difference implies flavor oscillations
Oscillation Length
sin 2(2𝜃)Probability
z
(𝜈𝑒
𝜈𝜇)=(c os𝜃 sin𝜃− sin 𝜃 c os 𝜃)(𝜈1𝜈2)
4𝜋 𝐸𝛿𝑚2 =2.5 m
𝐸MeV (eV𝛿𝑚
2
)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
• Japanese Nuclear Reactors 80 GW (20% world capacity)• Average distance 180 km• Flux 6 105 cm-2 s-1 • Without oscillations 2 captures per day
KamLAND Long-Baseline Reactor-Neutrino Experiment
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Oscillation of Reactor Neutrinos at KamLAND (Japan)Oscillation pattern for anti-electron neutrinos from
Japanese power reactors as a function of L/E
KamLAND Scintillatordetector (1000 t)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Atmospheric Neutrino AnomalyZenith-angle distribution of atmospheric neutrinosin Super-Kamiokande [hep-ex/0210019]
Half of the muon neutrinosfrom below are missing
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Long-Baseline Experiment K2K
K2K Experiment(KEK to Kamiokande)has confirmedneutrinooscillations,to be followedby T2K (2010)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Current Long-Baseline ExperimentsFermiLab–Soudan (MINOS) CERN – Gran Sasso
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
v
v
Three-Flavor Neutrino Parameters
(𝜈𝑒𝜈𝜇
𝜈𝜏)=(1 0 00 𝑐23 𝑠230 −𝑠23 𝑐23)(
𝑐13 0 𝑒−𝑖 𝛿𝑠130 1 0
−𝑒𝑖𝛿 𝑠13 0 𝑐13 )( 𝑐12 𝑠12 0−𝑠12 𝑐12 00 0 1)(
1 0 0
0 𝑒𝑖𝛼2
2 0
0 0 𝑒𝑖 𝛼3
2 )(𝜈1𝜈2𝜈3)Three mixing angles , , (Euler angles for 3D rotation), ,a CP-violating “Dirac phase” , and two “Majorana phases” and
⏟⏟⏟⏟39∘<𝜃23<53∘ 𝜃13<11∘ 33∘<𝜃12<37∘ Relevant for
0n2b decayAtmospheric/LBL-Beams Reactor Solar/KamLAND
me t
me t
m t
1Sun
Normal
2
3
Atmosphere
me t
me t
m t
1Sun
Inverted2
3
Atmosphere
72–80 meV2
2180–2640 meV2
Tasks and Open Questions• Precision for q12 and q23
• How large is q13 ?• CP-violating phase d ?• Mass ordering ? (normal vs inverted)• Absolute masses ? (hierarchical vs degenerate)• Dirac or Majorana ?
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Antineutrino Oscillations Different from Neutrinos?
Dirac phase causes different 3-flavor oscillationsfor neutrinos and antineutrinos
Distance [1000 km] for E = 1 GeV
same as
𝜈𝑒→𝜈𝜇
𝜈𝑒→𝜈𝜇
𝝂𝐞=𝑐12𝑐13𝝂𝟏+𝑠12𝑐13𝝂𝟐+𝑠13𝑒−𝑖 𝛿𝝂𝟑
𝝂𝐞=𝑐12𝑐13𝝂𝟏+𝑠12𝑐13𝝂𝟐+𝑠13𝑒+𝑖 𝛿𝝂𝟑
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrino CarabinerNamed for a subatomic particlewith almost zero mass, …
nGreek “nu”Now also in color
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
“Weighing” Neutrinos with KATRIN• Sensitive to common mass scale m for all flavors because of small mass differences from oscillations• Best limit from Mainz und Troitsk m < 2.2 eV (95% CL)• KATRIN can reach 0.2 eV• Under construction• Data taking foreseen to begin in 2012
http://www-ik.fzk.de/katrin/
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
“KATRIN Coming” (25 Nov 2006)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Pie Chart of Dark Universe
Dark Energy 73% (Cosmological Constant)
Neutrinos 0.1-2%
Dark Matter23%
Ordinary Matter 4%(of this only about 10% luminous)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Cosmological Limit on Neutrino Masses
JETP Lett. 4 (1966) 120
Cosmic neutrino “sea” 112 cm-3 neutrinos + anti-neutrinos per flavor
Ω𝜈h2=∑ 𝑚𝜈
93 eV<0.23
For allstable flavors∑𝑚𝜈≲20eV
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Weakly Interacting Particles as Dark Matter
Almost 40 years ago, beginnings of the idea of weakly interacting particles (neutrinos) as dark matter
Massive neutrinos are no longer a good candidate (hot dark matter)
However, the idea of weakly interacting massive particles (WIMPs) as dark matter is now standard
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
What is wrong with neutrino dark matter?Galactic Phase Space (“Tremaine-Gunn-Limit”)
Maximum mass density of a degenerateFermi gas
𝜌max=𝑚𝜈𝑝max3
3𝜋 2⏟𝑛max
=𝑚𝜈 (𝑚𝜈𝑣escape )
3
3𝜋 2
Spiral galaxies mn > 20–40 eVDwarf galaxies mn > 100–200 eV
Neutrino Free Streaming (Collisionless Phase Mixing)
NeutrinosNeutrinos
Over-density
• At T < 1 MeV neutrino scattering in early universe is ineffective• Stream freely until non-relativistic• Wash out density contrasts on small scales
• Neutrinos are “Hot Dark Matter”• Ruled out by structure formation
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Structure Formation with Hot Dark Matter
Neutrinos with Smn = 6.9 eVStandard LCDM Model
Structure fromation simulated with Gadget codeCube size 256 Mpc at zero redshift
Troels Haugbølle, http://users-phys.au.dk/haugboel
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Power Spectrum of Cosmic Density Fluctuations
Tegm
ark,
TAU
P 2
003
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Power Spectrum of CMB Temperature Fluctuations
Acoustic Peaks
Sky map of CMBR temperature fluctuations
Multipole expansion
Angular power spectrum
Δ (𝜃 ,𝜑 )=𝑇 (𝜃 ,𝜑 )− ⟨𝑇 ⟩⟨ 𝑇 ⟩
Δ (𝜃 ,𝜑 )=∑ℓ=0
∞
∑𝑚=−ℓ
ℓ
𝑎ℓ𝑚𝑌 ℓ𝑚 (𝜃 ,𝜑 )
𝐶ℓ= ⟨𝑎ℓ𝑚∗ 𝑎ℓ𝑚⟩= 12 ℓ+1 ∑𝑚=−ℓ
ℓ
𝑎ℓ𝑚∗ 𝑎ℓ𝑚
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Latest Angular Power Spectrum (WMAP 7 years)
Komatsu et al. (WMAP Collaboration), arXiv:1001.4538
Ratio 1st/3rd
peak fixes zeq
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Radiation Content at CMB Decoupling
• Existence of cosmic neutrino sea clearly confirmed by precision cosmology• All analyses find mild indication for excess radiation
• Planck data will fix Neff to ±0.26 (68% CL) or better
Komatsu et al. (WMAP Collaboration), arXiv:1001.4538
WMAP alone
+ Large-scale structure(LSS) and H0
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Weak Lensing - A Powerful Probe for the Future
Unlensed Lensed
Distortion of background images by foreground matter
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Mass-Energy-Inventory of the Universe
10-3 10-2 10-1 1 WAssuming h = 0.72
Luminous TotalBaryons
LDark Matter
1 10 eV
Tritium (Mainz/Troitsk)NeutrinosSuper-K
Future Tritium (KATRIN)
Weak lensing tomography
CMB & LSS
∑ 𝑚𝜈
310-2 10-1
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Are Neutrinos their own Antiparticles?
Matter
Quarks
-1/3 +2/3
d u
s c
tb
e
𝜈𝜏𝜏
Leptons
-1 0
1st Family
2nd Family
3rd Family
Charge
Weak Interaction
Strong Int’n
Electromagnetic Int’n
Gravitation
Anti-Leptons Anti-Quarks
𝜈𝜏
0
𝜏+¿ ¿
+1 -2/3
uct
+1/3
b
Anti-Matter
Strong Int’n
Electromagnetic Int’n
Much less anti-matter in the universe: Baryon asymmetry of the Universe (BAU)
0 0
„Majorana Neutrinos” are their own antiparticles
𝜈 e𝜈𝜇
𝜈𝜏
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Solar Neutrinos vs. Reactor Antineutrinos
Fissionable nucleus
Neutron
Nucleussplitting
Fission products w/ neutron excess
unstable nuclei effectively decay by
Detection by inverse decay
Reines and Cowan 1954–1956
Energy26.7 MeV
Ray Davis radiochemical detector (1967–1992)
Amounts to neutino capture by neutron
Does not work for reactor flux!
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Role of Neutrino Helicity (Handedness)Basic production processin reactors
Basic production processin the Sun
Cowan & Reines detectorin fast-moving rocket,overtakes small-mass solar
Majorana neutrinos:Helicity flip anti-neutrino property dependson Lorentz frame
Anti-neutrinos alwaysright-handed helicity
Neutrinos alwaysleft-handed helicity
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrinoless bb Decay
Some nuclei decay only bythe bb mode, e.g. Ge-76
76Ge76Se
76As
0+
2-
2+
0+
Half life 1021 yrStandard 2n mode 0n mode, enabled
by Majorana mass
|𝑚𝑒𝑒|=|∑𝑖=1𝑁
𝜆𝑖|𝑈 𝑒𝑖|2𝑚 𝑖|Measured
quantity
Best limitfrom 76Ge
|𝑚𝑒𝑒|<0.35eV
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
GERDA Germanium Double Beta Experiment Bare enriched Ge-76 array in liquid Ar,located in Gran Sasso
Phase I (being commissioned)18 kg (HdM/IGEX) + 15 kg natural Ge Test claim of Klapdor-Kleingrothaus
Phase II, O(100 kg years)Add 20 kg enriched new detectors Degenerate masses: 75–130 meV
Phase III, O(1000 kg years)with Majorana collaboration?1-ton scale Inverted hierarchy: 24–41 meV
Several other large projects worldwide
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
𝑚𝐷𝑚𝐷2 /𝑀 𝑀
See-Saw Model for Neutrino Masses
1027eV
Planckmass
GUTscale
Electroweak scale
QCDscale
Cosmologicalconstant
10241021101810151012109106103110− 3
(𝜈𝐿 ,𝑁𝑅 )( 0 𝑚𝐷
𝑚𝐷 𝑀 )( 𝜈𝐿
𝑁𝑅)
(𝜈𝐿 ,𝑁𝑅 )(𝑚𝐷2 /𝑀 00 𝑀 )( 𝜈𝐿
𝑁𝑅)
Mass matrix for one family of ordinary and heavy r.h. neutrinos
Diagonalization
One light and one heavy Majorana neutrino
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Leptogenesis by Majorana Neutrino Decays
Heavy sterileneutrino N
Lepton
Higgs
NN
ℓ
Φ
Φ
+
CP-violating decays ofheavy sterile neutrinos byinterference of tree-levelwith one-loop diagram
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Baryogenesis by Leptogenesis?
Dark Energy 73% (Cosmological Constant)
Neutrinos 0.1-2%
Dark Matter23%
Ordinary Matter 4%(of this only about 10% luminous)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Applied Neutrino Physics
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Reactor Monitoring
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrino Monitoring of Nuclear Reactors
Rea
ctor
Pow
er (%
)
-20
0
20
40
60
80
100
Date06/2005 10/2005 02/2006 06/2006 10/2006
Det
ecte
d A
ntin
eutr
inos
per
day
0
100
200
300
400
500
Predicted rate Reported powerObserved rate, 30 day average
Cycle 14Cycle 13outage
Cycle 13
San Onofre Nuclear Reactor(California)
Neutrino measurements withSONGS1 detector (1m3 Scintillator)
• 3.4 GW thermal power• Produces • 3800 neutrino reactions/day
in 1 m3 liquid scintillator
• Relatively small detectors can measure nuclear activity without intrusion• Of interest for monitoring by International Atomic Energy Agency (IAEA)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Geo Neutrinos: What is it all about?
We know surprisingly little aboutthe Earth’s interior• Deepest drill hole 12 km• Samples of crust for chemical analysis available (e.g. vulcanoes)• Reconstructed density profile from seismic measurements• Heat flux from measured temperature gradient 30-44 TW (Expectation from canonical BSE model 19 TW from crust and mantle, nothing from core)
• Neutrinos escape unscathed• Carry information about chemical composition, radioactive energy production or even a hypothetical reactor in the Earth’s core
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Geo NeutrinosExpected Geoneutrino Flux
Reactor Background
KamLAND Scintillator-Detector (1000 t)
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Latest KamLAND Measurements of Geo NeutrinosK. Inoue at Neutrino 2010
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
AAP 2011 Vienna
http://aap2011.in2p3.fr/
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Sanduleak -69 202Sanduleak -69 202
Large Magellanic Cloud Distance 50 kpc (160.000 light years)
Tarantula Nebula
Supernova 1987A23 February 1987
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrino Signal of Supernova 1987AKamiokande-II (Japan)Water Cherenkov detector2140 tonsClock uncertainty 1 min
Irvine-Michigan-Brookhaven (US)Water Cherenkov detector6800 tonsClock uncertainty 50 ms
Baksan Scintillator Telescope(Soviet Union), 200 tonsRandom event cluster 0.7/dayClock uncertainty +2/-54 s
Within clock uncertainties,all signals are contemporaneous
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
2002 Physics Nobel Prize for Neutrino Astronomy
Ray Davis Jr.(1914–2006)
Masatoshi Koshiba(*1926)
“for pioneering contributions to astrophysics, inparticular for the detection of cosmic neutrinos”
Crab Nebula
Physics Opportunities withSupernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München
2nd Schrödinger LectureTuesday, 10 May 2011, 16 ct
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Cosmic Rays
Air Shower: 1019 eV primary particle 100 billion secondary particles at sea level Victor Hess (1911/12)
100 years later we are still asking
What are the sourcesfor the primarycosmic rays?
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Neutrino Beams: Heaven and Earth
Target:Protons or Photons
Approx. equal fluxes ofphotons & neutrinos
Equal neutrino fluxesin all flavors due tooscillationsF. Halzen (2002)
𝜋 0
𝜸
𝜋±
𝝁𝝂𝝁
𝒆𝝂𝒆𝝂𝝁
𝝂𝒆𝝂𝝁𝝂𝝉
p
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Nucleus of the Active Galaxy NGC 4261
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Scott Amundsen Base at the South Pole
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
IceCube Neutrino Telescope at the South PoleInstrumentation of 1 km3 antarcticice with 5000 photo multiplierscompleted December 2010
Deep Core installed 2010Search for dark matter
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
IceCube Neutrino Sky
IceCube Collaboration, arXiv:1012.2137 and Gaisser at Neutel 2011
Full-sky map, based on 40 strings
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
ANTARES - Neutrino Telescope in the Mediterranean
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Luminescent Ceatures of the Deep Sea
40K2 min
P.Coyle, Neutel 2011
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Three Mediterranean Pilot Projects
NemoAntares
2500 m
3500 m 4500 m
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Towards a km3 Detector in the Mediterranean
http://www.km3net.org
Georg Raffelt, MPI Physics, Munich 1st Schrödinger Lecture, University Vienna, 5 May 2011
Frontiers of Neutrino Physics
Matter-Antimatter-Issues• Majorana masses (neutrinoless double beta decay)• Oscillation difference between and (Dirac phase)• Baryon asymmetry of the universe (leptogenesis)
Absolute Mass• Experimental determination• Role in cosmology for structure formation
Exploring the Universe with Neutrinos• Sources of high-energy cosmic rays• Next galactic supernova• Diffuse SN neutrino background in the universe• Sun• Earth• Reactor monitoring
Neutrinos at the center
n Astrophysics & Cosmology
Cosmic Rays
El
emen
tary
Par
ticle
Phy
sics