Title TU Darmstadt Physik Kolloquium 23 November 2007

Title TU Darmstadt, Physik Kolloquium, 23. November 2007 Neutrinos in Astrophysics and Cosmology Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Pauli’s Explanation of the Beta Decay Spectrum (1930) “Neutrino” (E. Fermi) Georg Raffelt, Max-Planck-Institut für Physik, München Niels Bohr: “Neutron” Energy not conserved Wolfgang Pauli (1930) (1900 -1958) in the quantum. Nobel domain? Prize 1945 Physik Kolloquium, 23. November 2007, TU Darmstadt

Periodic System of Elementary Particles Quarks Charge +2/3 Charge Leptons -1/3 Charge 1 st Family Up u Down d Electron 2 nd Family Charm c Strange s Muon 3 rd Family Top t Bottom Neutron b Tau -1 Charge 0 e e-Neutrino ne m m-Neutrino nm t t-Neutrino nt Gravitation Weak Interaction Proton (QED) Electromagnetic Interaction Strong Interaction (QCD) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Where do Neutrinos Appear in Nature? Nuclear Reactors Particle Accelerators Earth Atmosphere (Cosmic Rays) Earth Crust (Natural Radioactivity) Georg Raffelt, Max-Planck-Institut für Physik, München Supernovae (Stellar Collapse) SN 1987 A Astrophysical Accelerators Soon ? Cosmic Big Bang (Today 330 n/cm 3) Indirect Evidence Physik Kolloquium, 23. November 2007, TU Darmstadt

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, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Bethe’s Classic Paper on Nuclear Reactions in Stars No neutrinos from nuclear reactions in 1938 … Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Gamow & Schoenberg, Phys. Rev. 58: 1117 (1940) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

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, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

First Detection (1954 - 1956) Clyde Cowan (1919 – 1974) Anti-Electron Neutrinos from Hanford Nuclear Reactor Georg Raffelt, Max-Planck-Institut für Physik, München Fred Reines (1918 – 1998) Nobel prize 1995 n Detector prototype Cd g g p e+ e- 3 Gammas in coincidence g Physik Kolloquium, 23. November 2007, TU Darmstadt

First Measurement of Solar Neutrinos Inverse beta decay of chlorine 600 tons of Perchloroethylene Homestake solar neutrino observatory (1967 -2002) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Cherenkov Effect Light Elastic scattering or CC reaction Electron or Muon (Charged Particle) Light Cherenkov Ring Georg Raffelt, Max-Planck-Institut für Physik, München Ne utr ino Water Physik Kolloquium, 23. November 2007, TU Darmstadt

Super-Kamiokande Neutrino Detector 42 m 39. 3 m Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Super-Kamiokande: Sun in the Light of Neutrinos Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Solar Neutrino Spectrum 7 -Be line measured by Borexino (2007) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

BOREXINO • Neutrino electron scattering • Liquid scintillator technology (~ 300 tons) • Low energy threshold (~ 60 ke. V) • Online since 16 May 2007 • Expected without flavor oscillations 75 ± 4 c/100 t/d • Expected with oscillations 49 ± 4 c/100 t/d • BOREXINO result (August 07) 47 ± 7 stat ± 12 sys c/100 t/d Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Neutrino Flavor Oscillations Two-flavor mixing Each mass eigenstate propagates as with Phase difference Probability implies flavor oscillations ne nm sin 2(2 q) z Oscillation Length Georg Raffelt, Max-Planck-Institut für Physik, München Bruno Pontecorvo (1913 – 1993) Invented nu oscillations Physik Kolloquium, 23. November 2007, TU Darmstadt

Mixing of Neutrinos with Different Mass Neutrino mass m 1 Electron neutrino Neutrino mass m 2 Mass m 1 Mass m 2 > => m m 111 Neutrino propagation as a wave phenomenon Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Neutrino Oscillations Mass m 1 Mass m 2 > m 1 Georg Raffelt, Max-Planck-Institut für Physik, München Oscillation length Physik Kolloquium, 23. November 2007, TU Darmstadt

Neutrino Oscillations Oscillation length Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Three-Flavor Neutrino Parameters Atmospheric/K 2 K CHOOZ Solar/Kam. LAND 2 s ranges hep-ph/0405172 Solar 75 -92 Atmospheric 1400 -3000 d CP-violating phase 3 Normal m t Inverted m t e Sun m t e 2 1 Atmosphere 2 1 m t Sun m t e e 3 Georg Raffelt, Max-Planck-Institut für Physik, München m t 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 ? Physik Kolloquium, 23. November 2007, TU Darmstadt

Sanduleak -69 202 Supernova 1987 A 23 February 1987 Tarantula Nebula Large Magellanic Cloud Distance 50 kpc (160. 000 light years) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Crab Nebula Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Stellar Collapse and Supernova Explosion Main-sequence Onion structure star Degenerate iron core: r 109 g cm-3 Hydrogen Burning T 1010 K MFe 1. 5 Msun RFe 8000 km Georg Raffelt, Max-Planck-Institut für Physik, München Collapse (implosion) Helium-burning star Helium Burning Hydrogen Burning Physik Kolloquium, 23. November 2007, TU Darmstadt

Stellar Collapse and Supernova Explosion Newborn Neutron Star Collapse Explosion (implosion) ~ 50 km Neutrino Cooling Proto-Neutron Star r rnuc = 3 1014 g cm-3 T 30 Me. V Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Stellar Collapse and Supernova Explosion Newborn Neutron Star ~ 50 km Gravitational binding energy Eb 3 1053 erg 17% MSUN c 2 Neutrino Cooling Proto-Neutron Star r rnuc = 3 1014 g cm-3 T 30 Me. V Georg Raffelt, Max-Planck-Institut für Physik, München This shows up as 99% Neutrinos 1% Kinetic energy of explosion (1% of this into cosmic rays) 0. 01% Photons, outshine host galaxy Neutrino luminosity Ln 3 1053 erg / 3 sec 3 1019 LSUN While it lasts, outshines the entire visible universe Physik Kolloquium, 23. November 2007, TU Darmstadt

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 Baksan Scintillator Telescope (Soviet Union), 200 tons Random event cluster ~ 0. 7/day Clock uncertainty +2/-54 s Within clock uncertainties, signals are contemporaneous Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

SN 1987 A Event No. 9 in Kamiokande-II detector 2140 tons of water fiducial volume for SN 1987 A Hirata et al. , PRD 38 (1988) 448 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

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, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Neutrino-Driven Delayed Explosion Neutrino heating increases pressure behind shock front Picture adapted from Janka, astro-ph/0008432 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Standing Accretion Shock Instability (SASI) Mezzacappa et al. , http: //www. phy. ornl. gov/tsi/pages/simulations. html Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Large Detectors for Supernova Neutrinos Mini. Boo. NE (200) LVD (400) Borexino (100) Baksan (100) Ice. Cube (106) Georg Raffelt, Max-Planck-Institut für Physik, München Super-Kamiokande (104) Kam. LAND (400) In brackets events for a “fiducial SN” at distance 10 kpc Physik Kolloquium, 23. November 2007, TU Darmstadt

Simulated Supernova Signal at Super-Kamiokande Accretion Phase Kelvin-Helmholtz Cooling Phase Simulation for Super-Kamiokande SN signal at 10 kpc, based on a numerical Livermore model [Totani, Sato, Dalhed & Wilson, Ap. J 496 (1998) 216] Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Ice. Cube Neutrino Telescope at the South Pole • 1 km 3 antarctic ice, instrumented with 4800 photomultipliers • 22 of 80 strings installed (2007) • Completion until 2011 foreseen Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Global Cosmic Ray Spectrum Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Core of the Galaxy NGC 4261 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Ice. Cube as a Supernova Neutrino Detector Each optical module (OM) picks up Cherenkov light from its neighborhood. SN appears as “correlated noise”. • About 300 Cherenkov photons per OM from a SN at 10 kpc • Noise per OM < 260 Hz • Total of 4800 OMs in Ice. Cube Georg Raffelt, Max-Planck-Institut für Physik, München Ice. Cube SN signal at 10 kpc, based on a numerical Livermore model [Dighe, Keil & Raffelt, hep-ph/0303210] Method first discussed by • Pryor, Roos & Webster, Ap. J 329: 355 (1988) • Halzen, Jacobsen & Zas astro-ph/9512080 Physik Kolloquium, 23. November 2007, TU Darmstadt

H- and L-Resonance for MSW Oscillations R. Tomàs, M. Kachelriess, G. Raffelt, A. Dighe, H. -T. Janka & L. Scheck: Neutrino signatures of supernova forward and reverse shock propagation [astro-ph/0407132] Resonance density for Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Shock-Wave Propagation in Ice. Cube Inverted Hierarchy No shockwave Inverted Hierarchy Forward & reverse shock Inverted Hierarchy Forward shock Normal Hierarchy Choubey, Harries & Ross, “Probing neutrino oscillations from supernovae shock waves via the Ice. Cube detector”, astro-ph/0604300 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Core-Collapse SN Rate in the Milky Way SN statistics in external galaxies van den Bergh & Mc. Clure (1994) Cappellaro & Turatto (2000) Gamma rays from 26 Al (Milky Way) Diehl et al. (2006) Historical galactic SNe (all types) Strom (1994) Tammann et al. (1994) No galactic neutrino burst 90 % CL (25 y obserservation) Alekseev et al. (1993) 0 1 2 3 4 5 6 7 8 9 10 Core-collapse SNe per century References: van den Bergh & Mc. Clure, Ap. J 425 (1994) 205. Cappellaro & Turatto, astroph/0012455. Diehl et al. , Nature 439 (2006) 45. Strom, Astron. Astrophys. 288 (1994) L 1. Tammann et al. , Ap. J 92 (1994) 487. Alekeseev et al. , JETP 77 (1993) 339 and my update. Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Super. Nova Early Warning System (SNEWS) Neutrino observation can alert astronomers several hours in advance to a supernova. To avoid false alarms, require alarm from at least two experiments. Super-K Ice. Cube Supernova 1987 A Early Light Curve LVD Coincidence Server @ BNL Alert Others ? http: //snews. bnl. gov astro-ph/0406214 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

The Red Supergiant Betelgeuse (Alpha Orionis) First resolved image of a star other than Sun Distance (Hipparcos) 130 pc (425 lyr) If Betelgeuse goes Supernova: • 6 107 neutrino events in Super-Kamiokande • 2. 4 103 neutron events per day from Silicon-burning phase (few days warning!), need neutron tagging [Odrzywolek, Misiaszek & Kutschera, astro-ph/0311012] Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

LAGUNA - Funded FP 7 Design Study Large Apparati for Grand Unification and Neutrino Astrophysics (see also ar. Xiv: 0705. 0116) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Title Dark Energy 73% (Cosmological Constant) Normal Matter 4% (of this about 10% luminous) Georg Raffelt, Max-Planck-Institut für Physik, München Dark Matter 23% Neutrinos 0. 1 -2% Physik Kolloquium, 23. November 2007, TU Darmstadt

“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 2009 http: //www-ik. fzk. de/katrin/ Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

“KATRIN Approaching” (25 Nov 2006) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Cosmological Limit on Neutrino Masses Cosmic neutrino “sea” ~ 112 cm-3 neutrinos + anti-neutrinos per flavor mn < 40 e. V For all stable flavors A classic paper: Gershtein & Zeldovich JETP Lett. 4 (1966) 120 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Strukturbildung im Universum Smooth Structured Structure forms by gravitational instability of primordial density fluctuations A fraction of hot dark matter suppresses small-scale structure Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

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: //whome. phys. au. dk/~haugboel Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Power Spectrum of Cosmic Density Fluctuations Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Some Recent Cosmological Limits on Neutrino Masses Smn/e. V Data / Priors (limit 95%CL) Hannestad 2003 1. 01 [astro-ph/0303076] WMAP-1, CMB, 2 d. F, HST Spergel et al. (WMAP) 2003 0. 69 [astro-ph/0302209] WMAP-1, 2 d. F, HST, s 8 Crotty et al. 2004 [hep-ph/0402049] 1. 0 0. 6 WMAP-1, CMB, 2 d. F, SDSS & HST, SN Hannestad 2004 [hep-ph/0409108] 0. 65 WMAP-1, SDSS, SN Ia gold sample, Ly-a data from Keck sample Seljak et al. 2004 0. 42 [astro-ph/0407372] WMAP-1, SDSS, Bias, Ly-a data from SDSS sample Hannestad et al. 2006 [hep-ph/0409108] 0. 30 WMAP-1, CMB-small, SDSS, 2 d. F, SN Ia, BAO (SDSS), Ly-a (SDSS) Spergel et al. 2006 [hep-ph/0409108] 0. 68 WMAP-3, SDSS, 2 d. F, SN Ia, s 8 Seljak et al. 2006 0. 14 [astro-ph/0604335] Georg Raffelt, Max-Planck-Institut für Physik, München WMAP-3, CMB-small, SDSS, 2 d. F, SN Ia, BAO (SDSS), Ly-a (SDSS) Physik Kolloquium, 23. November 2007, TU Darmstadt

Fermion Mass Spectrum Quarks (Q = -1/3) d Quarks (Q = +2/3) Charged Leptons (Q = -1) All flavors n 3 s u e b c m t t Neutrinos 1 10 100 1 10 100 1 me. V ke. V Me. V Ge. V Te. V Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Periodic System of Elementary Particles Matter Antimatter „Majorana Neutrinos” are their own antiparticles Why is there no antimatter Can explain baryogenesis in the Universe? by leptogenesis (Problem of „Baryogenesis”) Quarks Charge +2/3 Leptons -1/3 -1 1 st Family u d e 2 nd Family c s m 3 rd Family t b t 0 Anti-Leptons 0 0 +1 Anti-Quarks +1/3 -2/3 Gravitation Weak Interaction Electromagnetic Int’n Strong Int’n Georg Raffelt, Max-Planck-Institut für Physik, München Electromagnetic Int’n Strong Int’n Physik Kolloquium, 23. November 2007, TU Darmstadt

See-Saw Model for Neutrino Masses Charged Leptons Dirac masses from coupling to standard Higgs field f Neutrinos Heavy Majorana masses Mj > 1010 Ge. V Lagrangian for particle masses Light Majorana mass Diagonalize Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

See-Saw Model for Neutrino Masses n ℓ N Heavy “right-handed” neutrinos (no gauge interactions) Charged leptons 1010 Ge. V 1 Ge. V Georg Raffelt, Max-Planck-Institut für Physik, München Ordinary neutrinos Light Majorana mass 10 -10 Ge. V Physik Kolloquium, 23. November 2007, TU Darmstadt

Leptogenesis by Out-of-Equilibrium Decay Equilibrium abundance of heavy Majorana neutrinos Real abundance determined by decay rate M. Fukugita & T. Yanagida: Baryogenesis without Grand Unification Phys. Lett. B 174 (1986) 45 CP-violating decays by interference of tree-level with one-loop diagram Created lepton-number abundance W. Buchmüller & M. Plümacher: Neutrino masses and the baryon asymmetry Int. J. Mod. Phys. A 15 (2000) 5047 -5086 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Leptogenesis by Majorana Neutrino Decays In see-saw models for neutrino masses, out-of-equilibrium decays of right-handed heavy Majorana neutrinos provide source for CP- and L-violation Cosmological evolution • B = L = 0 early on • Thermal freeze-out of heavy Majorana neutrinos • Out-of-equilibrium CP-violating decay creates net L • Shift L excess into B by sphaleron effects Sufficient deviation from equilibrium distribution of heavy Majorana neutrinos at freeze-out Limits on Yukawa couplings Limits on masses of ordinary neutrinos Requires Majorana neutrino masses below 0. 1 e. V Buchmüller, Di Bari & Plümacher, hep-ph/0209301 & hep-ph/0302092 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Title Dark Energy 73% (Cosmological Constant) Normal Matter 4% (of this about 10% luminous) Georg Raffelt, Max-Planck-Institut für Physik, München Massive neutrinos can explain presence of matter by leptogenesis mechanism Dark Matter 23% Neutrinos 0. 1 -2% Physik Kolloquium, 23. November 2007, TU Darmstadt

Killing Two Birds with One Stone See-Saw mechanism explains • Small neutrino masses • Baryon asymmetry of the universe by leptogenesis Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Leptogenesis by Majorana Neutrino Decays A classic paper Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Leptogenesis as a Research Topic Citation of Fukugita & Yanagida, PLB 174 (1986) 45 or “leptogenesis” in title (SPIRES data base) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Elementary Particle Physics Portion of the Hubble Ultra Deep Field Georg Raffelt, Max-Planck-Institut für Physik, München Ast rop hy sic s& n Co sm olo gy s y a R c i m s Co Physik Kolloquium, 23. November 2007, TU Darmstadt

Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Gamow & Schoenberg 2 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Long-Baseline Experiment K 2 K Experiment (KEK to Kamiokande) has confirmed neutrino oscillations, to be followed by T 2 K (2009) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Geo Neutrinos Predicted geo neutrino flux Kam. LAND scintillator detector (1 kton) Reactor background Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Matrices of Density in Flavor Space Neutrino quantum field Spinors in flavor space Destruction operators for (anti)neutrinos Variables for discussing neutrino flavor oscillations Quantum states (amplitudes) “Matrices of densities” (analogous to occupation numbers) Neutrinos Antineutrinos Sufficient for “beam experiments, ” but confusing “wave packet debates” for quantifying decoherence effects Georg Raffelt, Max-Planck-Institut für Physik, München “Quadratic” quantities, required for dealing with decoherence, collisions, Pauli-blocking, nu-nu-refraction, etc. Physik Kolloquium, 23. November 2007, TU Darmstadt

General Equations of Motion • Vacuum oscillations M is neutrino mass matrix Usual matter effect with • Note opposite sign between neutrinos and antineutrinos Nonlinear nu-nu effects are important when nu-nu interaction energy exceeds typical vacuum oscillation frequency (Do not compare with matter effect!) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Toy Supernova in “Single-Angle” Approximation • Assume 80% anti-neutrinos • Vacuum oscillation frequency w = 0. 3 km-1 • Neutrino-neutrino interaction energy at nu sphere (r = 10 km) m = 0. 3 105 km-1 • Falls off approximately as r-4 (geometric flux dilution and nus become more co-linear) Bipolar Oscillations Decline of oscillation amplitude explained in pendulum analogy by inreasing moment of inertia (Hannestad, Raffelt, Sigl & Wong astro-ph/0608695) Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Collective SN neutrino oscillations 2006 -2007 “Bipolar” collective transformations important, even for dense matter • Duan, Fuller & Qian astro-ph/0511275 Numerical simulations • Including multi-angle effects • Discovery of “spectral splits” • Duan, Fuller, Carlson & Qian astro-ph/0606616, 0608050 • Pendulum in flavor space • Collective pair annihilation • Pure precession mode • Hannestad, Raffelt, Sigl & Wong astro-ph/0608695 • Duan, Fuller, Carlson & Qian astro-ph/0703776 Self-maintained coherence vs. self-induced decoherence caused by multi-angle effects • Raffelt & Sigl, hep-ph/0701182 • Esteban-Pretel, Pastor, Tomas, Raffelt & Sigl, ar. Xiv: 0706. 2498 Theory of “spectral splits” in terms of adiabatic evolution in rotating frame • Raffelt & Smirnov, ar. Xiv: 0705. 1830, 0709. 4641 • Duan, Fuller, Carlson & Qian ar. Xiv: 0706. 4293, 0707. 0290 Independent numerical simulations • Fogli, Lisi, Marrone & Mirizzi ar. Xiv: 0707. 1998 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

SN 1006 Looking forward to the next galactic supernova Georg Raffelt, Max-Planck-Institut für Physik, München http: //antwrp. gsfc. nasa. gov/apod/ap 060430. html Physik Kolloquium, 23. November 2007, TU Darmstadt

Delayed Explosion Wilson, Proc. Univ. Illinois Meeting on Num. Astrophys. (1982) Bethe & Wilson, Ap. J 295 (1985) 14 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Experimental Limits on Relic Supernova Neutrinos Super-K upper limit 29 cm-2 s-1 for Kaplinghat et al. spectrum [hep-ex/0209028] Upper-limit flux of Kaplinghat et al. , astro-ph/9912391 Integrated 54 cm-2 s-1 Cline, astro-ph/0103138 Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

DSNB Measurement with Neutron Tagging Beacom & Vagins, hep-ph/0309300 [Phys. Rev. Lett. , 93: 171101, 2004] Future large-scale scintillator detectors (e. g. LENA with 50 kt) • Inverse beta decay reaction tagged • Location with smaller reactor flux (e. g. Pyhäsalmi in Finland) could allow for lower threshold Pushing the boundaries of neutrino astronomy to cosmological distances Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Neutrinos in Astrophysics and Cosmology Neutrinos responsible for ordinary astrophysical and cosmological phenomena • Dominant radiation component in the early universe • Crucial role in big-bang nucleosynthesis • Dark-matter component (but subdominant) • May be responsible for baryonic matter in the universe (leptogenesis) • Important (sometimes dominant) cooling agent of stars • May trigger supernova explosions • May be crucial for r-process nucleosynthesis Heavenly laboratories for new particle physics phenomena • Cosmological limit (future detection? ) of nu mass scale • Flavor oscillations of solar and atmospheric neutrinos • Neutrino oscillations from a future galactic supernova • Limits on “exotic” neutrino properties (dipole moments, right-handed interactions, decays, flavor-violating neutral currents, sterile nus, …) Neutrinos as astrophysical messengers • Look into the solar interior (“measure” temperature) • Watch stellar collapse directly • Neutrinos from all cosmological supernovae • Astrophysical accelerators for cosmic rays • Annihilation signature for neutralino dark matter Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

Hot dark matter ruled out in 1983 1000 particle simulation [Frenk, White & Davis, Ap. J 271 (1983) 417] The coherence length of the neutrino distribution […] is too large to be consistent with the observed clustering scale of galaxies […] The conventional neutrino-dominated picture appears to be ruled out. White, Frenk & Davis, Ap. J 274 (1983) L 1. Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt