Neutrinos Ghost Particles of the Universe Neutrinos Ghost

Neutrinos – Ghost Particles of the Universe Neutrinos Ghost Particles of the Universe Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany 1 Schrödinger Lecture, University Vienna, 5 May 2011 Georg Raffelt, MPI Physics, Munich st

Periodic System of Elementary Particles Quarks Charge -1/3 Charge Leptons +2/3 Charge -1 Charge 0 1 st Family Down d Up u Electron e e-Neutrino ne 2 nd Family Strange s Charm c Muon m m-Neutrino nm 3 rd Family Bottom b Top Neutron t Tau t t-Neutrino nt Strong Interaction (8 Gluons) Electromagnetic Interaction (Photon) Weak Interaction (WProton and Z Bosons) Gravitation (Gravitons? ) Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Where do Neutrinos Appear in Nature? Nuclear Reactors Particle Accelerators Earth Atmosphere (Cosmic Rays) Earth Crust (Natural Radioactivity) Sun Supernovae (Stellar Collapse) SN 1987 A Astrophysical Accelerators Soon ? Cosmic Big Bang (Today 330 n/cm 3) Indirect Evidence

Pauli’s Explanation of the Beta Decay Spectrum (1930) “Neutrino” (E. Fermi) Georg Raffelt, MPI Physics, Munich “Neutron” (1930) Niels Bohr: Energy not conserved in the quantum Wolfgang domain? Pauli (1900– 1958) Nobel Prize 1945 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Neutrinos from the Sun Helium Reactionchains Energy 26. 7 Me. V Solar radiation: 98 % light 2 % neutrinos At Earth 66 billion neutrinos/cm 2 sec Hans Bethe (1906 -2005, Nobel prize 1967) Thermonuclear reaction chains (1938) Georg Raffelt, MPI Physics, Munich 1 st 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 1 st Schrödinger Lecture, University Vienna, 5 May 2011

First Detection (1954 – 1956) Clyde Cowan (1919 – 1974) Anti-Electron Neutrinos from Hanford Nuclear Reactor Georg Raffelt, MPI Physics, Munich Fred Reines (1918 – 1998) Nobel prize 1995 n p Detector prototype Cd g g 3 Gammas in coincidence g 1 st Schrödinger Lecture, University Vienna, 5 May 2011

First Measurement of Solar Neutrinos Inverse beta decay of chlorine 600 tons of Perchloroethylene Homestake solar neutrino observatory (1967– 2002) Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Cherenkov Effect Elastic scattering or CC reaction Light Electron or Muon (Charged Particle) Light Cherenkov Ring Ne utr ino Water

Super-Kamiokande Neutrino Detector (Since 1996) 42 m 39. 3 m Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Super-Kamiokande: Sun in the Light of Neutrinos

Neutrino Flavor Oscillations Two-flavor mixing Bruno Pontecorvo (1913– 1993) Invented nu oscillations z Oscillation Length Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Kam. LAND Long-Baseline Reactor-Neutrino Experiment Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Oscillation of Reactor Neutrinos at Kam. LAND (Japan) Oscillation pattern for anti-electron neutrinos from Japanese power reactors as a function of L/E Kam. LAND Scintillator detector (1000 t) Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Atmospheric Neutrino Anomaly Zenith-angle distribution of atmospheric neutrinos in Super-Kamiokande [hep-ex/0210019] Half of the muon neutrinos from below are missing Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Long-Baseline Experiment K 2 K Experiment (KEK to Kamiokande) has confirmed neutrino oscillations, to be followed by T 2 K (2010) Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Current Long-Baseline Experiments Fermi. Lab–Soudan (MINOS) Georg Raffelt, MPI Physics, Munich CERN – Gran Sasso 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Three-Flavor Neutrino Parameters v Reactor Atmospheric/LBL-Beams Normal 3 m t Inverted 2 1 m t Sun e m t e Atmosphere v Atmosphere 2 1 m t Sun e m t Solar/Kam. LAND e 3 Georg Raffelt, MPI Physics, Munich m t 2180– 2640 me. V 2 Relevant for 0 n 2 b decay Tasks and Open Questions • Precision for q 12 and q 23 • How large is q 13 ? • CP-violating phase d ? • Mass ordering ? (normal vs inverted) • Absolute masses ? (hierarchical vs degenerate) • Dirac or Majorana ? 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Antineutrino Oscillations Different from Neutrinos? Dirac phase causes different 3 -flavor oscillations for neutrinos and antineutrinos Distance [1000 km] for E = 1 Ge. V Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Neutrino Carabiner Named for a subatomic particle with almost zero mass, … n Now also in color Greek “nu” Georg Raffelt, MPI Physics, Munich 1 st 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 e. V (95% CL) • KATRIN can reach 0. 2 e. V • Under construction • Data taking foreseen to begin in 2012 http: //www-ik. fzk. de/katrin/ Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

“KATRIN Coming” (25 Nov 2006) Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Pie Chart of Dark Universe Dark Energy 73% (Cosmological Constant) Ordinary Matter 4% (of this only about 10% luminous) Georg Raffelt, MPI Physics, Munich Dark Matter 23% Neutrinos 0. 1 -2% 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Cosmological Limit on Neutrino Masses For all stable flavors JETP Lett. 4 (1966) 120 Georg Raffelt, MPI Physics, Munich 1 st 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 1 st 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 degenerate Fermi gas Spiral galaxies mn > 20– 40 e. V Dwarf galaxies mn > 100– 200 e. V Neutrino Free Streaming (Collisionless Phase Mixing) • At T < 1 Me. V neutrino scattering in early universe is ineffective • Stream freely until non-relativistic • Wash out density contrasts on small scales Neutrinos Over-density Georg Raffelt, MPI Physics, Munich • Neutrinos are “Hot Dark Matter” • Ruled out by structure formation 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Structure Formation with Hot Dark Matter Standard LCDM Model Neutrinos with Smn = 6. 9 e. V Structure fromation simulated with Gadget code Cube size 256 Mpc at zero redshift Troels Haugbølle, http: //users-phys. au. dk/haugboel Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Tegmark, TAUP 2003 Power Spectrum of Cosmic Density Fluctuations Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Power Spectrum of CMB Temperature Fluctuations Sky map of CMBR temperature fluctuations Multipole expansion Acoustic Peaks Angular power spectrum Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Latest Angular Power Spectrum (WMAP 7 years) Ratio 1 st/3 rd peak fixes zeq Komatsu et al. (WMAP Collaboration), ar. Xiv: 1001. 4538 Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Radiation Content at CMB Decoupling WMAP alone + Large-scale structure (LSS) and H 0 Komatsu et al. (WMAP Collaboration), ar. Xiv: 1001. 4538 • 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 Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Weak Lensing - A Powerful Probe for the Future Distortion of background images by foreground matter Unlensed Georg Raffelt, MPI Physics, Munich Lensed 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Mass-Energy-Inventory of the Universe Assuming h = 0. 72 10 -3 10 -2 10 -1 1 Baryons Luminous Total L Dark Matter 10 -2 10 -1 1 Super-K Neutrinos W 10 e. V Tritium (Mainz/Troitsk) Future Tritium (KATRIN) CMB & LSS Weak lensing tomography Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Are Neutrinos their own Antiparticles? Matter Anti-Matter „Majorana Neutrinos” Much less anti-matter in the universe: Baryon asymmetry are their own antiparticles of the Universe (BAU) Quarks Anti-Leptons -1/3 +2/3 -1 1 st Family d u e 2 nd Family s c 3 rd Family b t Charge Strong Int’n Electromagnetic Int’n 0 0 +1 Anti-Quarks -2/3 +1/3 Strong Int’n Electromagnetic Int’n Weak Interaction Gravitation Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Solar Neutrinos vs. Reactor Antineutrinos Neutron Fissionable nucleus Energy 26. 7 Me. V Ray Davis radiochemical detector (1967– 1992) Nucleus splitting Fission products w/ neutron excess Amounts to neutino capture by neutron Reines and Cowan 1954– 1956 Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Role of Neutrino Helicity (Handedness) Basic production process in reactors Anti-neutrinos always right-handed helicity Basic production process in the Sun Neutrinos always left-handed helicity Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Neutrinoless bb Decay Some nuclei decay only by the bb mode, e. g. Ge-76 76 As 0+ 76 Ge 276 Se 2+ 0+ Standard 2 n mode 0 n mode, enabled by Majorana mass Measured quantity Best limit from 76 Ge Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

GERDA Germanium Double Beta Experiment Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

See-Saw Model for Neutrino Masses Cosmological constant QCD Electroweak scale GUT scale Planck mass e. V 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 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Leptogenesis by Majorana Neutrino Decays Heavy sterile neutrino N Georg Raffelt, MPI Physics, Munich + N N CP-violating decays of heavy sterile neutrinos by interference of tree-level with one-loop diagram 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Baryogenesis by Leptogenesis? Dark Energy 73% (Cosmological Constant) Ordinary Matter 4% (of this only about 10% luminous) Georg Raffelt, MPI Physics, Munich Dark Matter 23% Neutrinos 0. 1 -2% 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Applied Neutrino Physics Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Reactor Monitoring Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Neutrino Monitoring of Nuclear Reactors San Onofre Nuclear Reactor (California) Neutrino measurements with SONGS 1 detector (1 m 3 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 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Geo Neutrinos: What is it all about? • 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 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Geo Neutrinos Expected Geoneutrino Flux Kam. LAND Scintillator-Detector (1000 t) Reactor Background Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Latest Kam. LAND Measurements of Geo Neutrinos K. Inoue at Neutrino 2010 Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

AAP 2011 Vienna Georg Raffelt, MPI Physics, Munich http: //aap 2011. in 2 p 3. fr/ 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Sanduleak -69 202 Supernova 1987 A Sanduleak -69 202 23 February 1987 Tarantula Nebula Large Magellanic Cloud Distance 50 kpc (160. 000 light years) Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Neutrino Signal of Supernova 1987 A Kamiokande-II (Japan) Water Cherenkov detector 2140 tons Clock uncertainty 1 min Irvine-Michigan-Brookhaven (US) Water Cherenkov detector 6800 tons Clock uncertainty 50 ms Within clock uncertainties, all signals are contemporaneous Georg Raffelt, MPI Physics, Munich 1 st 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, in particular for the detection of cosmic neutrinos” Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Crab Nebula 2 nd Schr ödinger Lecture Tuesday, 10 May 2011, 16 ct Physics Opportunities with Supernova Neutrinos Georg Raffelt, Max-Planck-Institut für Physik, München

Cosmic Rays 100 years later we are still asking What are the sources for the primary cosmic rays? Air Shower: § 1019 e. V primary particle § 100 billion secondary Victor Hess (1911/12) particles at sea level Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Neutrino Beams: Heaven and Earth p Target: Protons or Photons Approx. equal fluxes of photons & neutrinos F. Halzen (2002) Georg Raffelt, MPI Physics, Munich Equal neutrino fluxes in all flavors due to oscillations 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Nucleus of the Active Galaxy NGC 4261 Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Scott Amundsen Base at the South Pole Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Ice. Cube Neutrino Telescope at the South Pole Deep Core installed 2010 Search for dark matter Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Ice. Cube Neutrino Sky Full-sky map, based on 40 strings Ice. Cube Collaboration, ar. Xiv: 1012. 2137 and Gaisser at Neutel 2011 Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

ANTARES - Neutrino Telescope in the Mediterranean Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Luminescent Ceatures of the Deep Sea P. Coyle, Neutel 2011 40 K 2 min Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Three Mediterranean Pilot Projects 2500 m 3500 m 4500 m Antares Nemo Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Towards a km 3 Detector in the Mediterranean http: //www. km 3 net. org Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Frontiers of Neutrino Physics Georg Raffelt, MPI Physics, Munich 1 st Schrödinger Lecture, University Vienna, 5 May 2011

Elementary Particle Physics Neutrinos at the center Ast rop hys ics & n Co sm olo gy ys a c. R i sm o C