Neutrino Sources in the Universe

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1 Crab Nebula Neutrino Sources in the Universe Georg G. Raffelt Max-Planck-Institut für Physik, München

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

3 Grand Unified Neutrino Spectrum Georg Raffelt, MPI Physik, München Slide adapted from Christian Spiering Sino-German GDT Symposium, Ringberg Castle, 19 Oct 2015

4 Grand Unified Neutrino Spectrum underground optical: - deep water - deep ice - air showers - radio - acoustics Georg Raffelt, MPI Physik, München Slide adapted from Christian Spiering Sino-German GDT Symposium, Ringberg Castle, 19 Oct 2015

5 Missing Solar Neutrinos in Many Experiments Chlorine Gallium Water n e + e n e + e Heavy Water n e + d p + p + e 8 B CNO 8 B 7 Be 8 B 8 B CNO 7 Be pp Homestake Gallex/GNO SAGE (Super-) Kamiokande SNO

6 Neutrino Flavor Oscillations Pontecorvo & Gribov (1968) on the Solar Neutrino Problem Neutrinos are superposition of mass eigenstates ν e = +cos Θ ν 1 + sin Θ ν 2 ν μ = sin Θ ν 1 + cos Θ ν 2 Different speed of propagation Phase difference δm2 L causes oscillations 2E Similar to optical activity in the propagation of light Probability ν e ν μ Bruno Pontecorvo ( ) sin 2 (2θ) L Oscillation Length 4πE δm 2 = 2.5 m E MeV ev 2 δm 2 Vladimir Gribov ( )

7 SNO Proposal Herbert Hwa Chen ( ) Proposal 1984: Heavy water as target Can see all neutrino flavors Available in Canada as a loan from strategic reserve of CANDU reactor programme Formation of Sudbury Neutrino Observatory project (SNO) H. Chen passes away on 7. Nov and Art McDonald (then Princeton) takes on leadership Measurement of the full solar neutrino flux in 2002 Nobel prize for Art McDonald 2015

8 Sudbury Neutrino Observatory (SNO) tons of heavy water Normal (light) water H 2 0 Heavy water D 2 0 Nucleus of hydrogen (proton) Nucleus of heavy hydrogen (deuterium)

9 Sudbury Neutrino Observatory (SNO) tons of heavy water Normal (light) water H 2 0 Heavy water D 2 0 Nucleus of hydrogen (proton) Nucleus of heavy hydrogen (deuterium)

10 Sudbury Neutrino Observatory (SNO) tons of heavy water Normal (light) water H 2 0 Heavy water D 2 0 Nucleus of hydrogen (proton) Nucleus of heavy hydrogen (deuterium)

11 Sudbury Neutrino Observatory (SNO) Heavy hydrogen (deuterium) Heavy hydrogen (deuterium) Electron neutrinos All neutrino flavors

12 SNO Results (2002) Missing electron neutrinos indeed arrive in the form of other flavors! Phys. Rev. Lett. 89:011301, 2002 (

13 SNO Results (2002) Missing electron neutrinos indeed arrive in the form of other flavors! Arthur McDonald Queen s University, Canada Phys. Rev. Lett. 89:011301, 2002 (

14 Reactor Neutrino Oscillations (KamLAND, Japan) Oscillation pattern for anti-electron-neutrinos as a function of energy at fixed distance (ca 180 km) ν e survival probability Measurements Expected survival probability based on reactor distances Distance/energy (km/mev) KamLAND Scintillator-Detector (1000 t)

15 Reactor- and Geo-Neutrinos in KamLAND (Japan) Overall Geo-neutrinos (plus in Borexino) Earthquake & Tsunami (2011) All reactors switched off Counts per day Backgrounds Neutrinos from reactors Measurements (adaptiert) Year Scintillator purification Building KamLAND-Zen Beginning of geophysics with neutrinos!

16 Plate Tectonics, Convection, Geo-Dynamo Potassium-40 (Half life 1.25 billion years) Thorium-232 (14 billion years) Uranium-238 (4.5 billion years) Radioactive decays are the driving force!

17 Geo-Neutrino Fluss Glenn Jocher (Neutrino Geoscience, Paris 2015)

18 SNO+ (800 t) to begin 2016 Borexino (300 t) Geo-Neutrino Detektoren KamLAND since 2007 (1000 t) since 2002 Hanohano ( t) For oceanic crust (Idea of principle, not a project) JUNO ( t) to begin 2020

19 Crab Nebula Remnant of SN 1054 Crab Nebula Remnant of SN 1054 Chinese Supernova Crab Pulsar Chandra x-ray images

20 Stellar Collapse and Supernova Explosion Main-sequence star Helium-burning star Hydrogen Burning Helium Burning Hydrogen Burning

21 Stellar Collapse and Supernova Explosion Main-sequence Onion structure star Collapse Helium-burning (implosion) star Degenerate iron core: r 10 9 g cm -3 T K M Fe 1.5 M sun R Fe 3000 km Hydrogen Burning Helium Burning Hydrogen Burning

22 Stellar Collapse and Supernova Explosion Newborn Neutron Star Collapse Explosion (implosion) ~ 50 km Proto-Neutron Star r ~ r nuc = g cm -3 T ~ 10 MeV

23 Stellar Collapse and Supernova Explosion Newborn Neutron Star ~ 50 km Gravitational binding energy E b erg 17% M SUN c 2 Neutrino cooling by diffusion This shows up as 99% Neutrinos 1% Kinetic energy of explosion 0.01% Photons, outshine host galaxy Neutrino luminosity Proto-Neutron Star r ~ r nuc = g cm -3 T ~ 10 MeV L n ~ erg / 3 sec ~ L SUN While it lasts, outshines the entire visible universe

24 Exploding 3D Garching Model (20 M SUN ) Melson, Janka, Bollig, Hanke, Marek & Müller, arxiv:

25 Variability to be seen in Neutrinos (3D Model) Tamborra, Hanke, Müller, Janka & Raffelt, arxiv: See also Lund, Marek, Lunardini, Janka & Raffelt, arxiv:

26 Sanduleak Sanduleak Tarantula Nebula Large Magellanic Cloud Distance 50 kpc ( light years)

27 Sanduleak Sanduleak Supernova 1987A 23 February 1987 Tarantula Nebula Large Magellanic Cloud Distance 50 kpc ( light years)

28 Neutrino Signal of Supernova 1987A 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 (Russia) 200 tons Random event cluster ~ 0.7/day Clock uncertainty +2/-54 s Within clock uncertainties, all signals are contemporaneous

29 Operational Detectors for Supernova Neutrinos SNO+ (300) HALO (tens) LVD (400) Borexino (100) Baksan (100) Super-K (10 4 ) KamLAND (400) Daya Bay (100) IceCube (10 6 ) In brackets events for a fiducial SN at distance 10 kpc

30 IceCube Neutrino Telescope at the South Pole Digital Optical Module

31 Three Types of High-Energy Messengers Cosmic rays (charged particles) Gamma Rays Neutrinos

32 Discovery of the Year (2013)

33 Astrophysical IceCube Neutrinos No clear astrophysical sources more neutrinos needed!

34 Global Neutrino Network (GNN) Antares KM3NeT GVD IceCube Gen-2

35 Neutrinos at the center