Crab Nebula Neutrinos in Astrophysics and Cosmology Neutrinos

Crab Nebula Neutrinos in Astrophysics and Cosmology Neutrinos from the Sun Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014 Georg Raffelt, MPI Physics, Munich

Neutrinos from the Sun Helium Reactionchains Energy 26. 7 Me. V Solar radiation: 98 % light (photons) 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 Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Hydrogen Burning: Proton-Proton Chains < 0. 420 Me. V 1. 442 Me. V 100% 0. 24% PP-I 85% 90% 15% hep 10% 0. 862 Me. V < 18. 8 Me. V 0. 02% 0. 384 Me. V < 15 Me. V PP-II Georg Raffelt, MPI Physics, Munich PP-III Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Neutrino Spectrum Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

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 Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Results of Chlorine Experiment (Homestake) Ap. J 496: 505, 1998 Theoretical Expectation Average Rate Average (1970 -1994) 2. 56 0. 16 stat 0. 16 sys SNU (SNU = Solar Neutrino Unit = 1 Absorption / sec / 1036 Atoms) Theoretical Prediction 6 -9 SNU “Solar Neutrino Problem” since 1968 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

GALLEX/GNO and SAGE Inverse Beta Decay Gallium Germanium GALLEX/GNO (1991– 2003) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Gallium Results Shown at Neutrino 2006 Gavrin, Phys. At. Nucl. 76 (2013) 1238 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Sudbury Neutrino Observatory (SNO) 1999– 2006 1000 tons of heavy water Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Sudbury Neutrino Observatory (SNO) 1999– 2006 1000 tons of heavy water Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Sudbury Neutrino Observatory (SNO) 1999– 2006 1000 tons of heavy water Normal (light) water H 20 Heavy water D 20 Nucleus of hydrogen (proton) Nucleus of heavy hydrogen (deuterium) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Sudbury Neutrino Observatory (SNO) 1999– 2006 Heavy hydrogen (deuterium) Electron neutrinos Georg Raffelt, MPI Physics, Munich Heavy hydrogen (deuterium) All neutrino flavors Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Missing Neutrinos from the Sun All Flavors Electron-Neutrino Detectors Chlorine Gallium Water -- n + e nn + e e+ e n e + e Heavy Water ne+ d p + e- Heavy Water n + d p + n 8 B CNO 8 B 7 Be 8 B pp CNO 7 Be Homestake 8 B 8 B Gallex/GNO SAGE Georg Raffelt, MPI Physics, Munich (Super-) Kamiokande SNO Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Charged and Neutral-Current SNO Measurements Ahmad et al. (SNO Collaboration), PRL 89: 011301, 2002 (nucl-ex/0204008) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Neutrino Spectrum Be-7 line measured by Borexino (2007) pep line measured by Borexino (2011) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Neutrino Spectroscopy with BOREXINO Shoulder in e recoil spectrum • Expected without flavor oscillations 75 ± 4 counts/100 t/d • Expected with oscillations 49 ± 4 counts/100 t/d • BOREXINO result (May 2008) 49 ± 3 stat ± 4 sys cnts/100 t/d ar. Xiv: 0805. 3843 (25 May 2008) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

pep Neutrinos in Borexino Collaboration, ar. Xiv: 1110. 3230 v 1 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

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 Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Best-fit “solar” oscillation parameters Yusuke Koshio at Neutrino 2014 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Three-Flavor Neutrino Parameters v Atmospheric/LBL-Beams Normal 3 m t Reactor Solar/Kam. LAND Inverted 2 1 m t Solar e m t e Atmospheric 1 m t Solar e m t Relevant for 0 n 2 b decay Tasks and Open Questions • Precision for all angles • CP-violating phase d ? • Mass ordering ? (normal vs inverted) • Absolute masses ? (hierarchical vs degenerate) • Dirac or Majorana ? Atmospheric 2 e 2180– 2640 me. V 2 3 Georg Raffelt, MPI Physics, Munich m t Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Matter Effect on Flavor Oscillations in the Sun Low energy (E ≲ 1 Me. V) Phase-averaged vacuum oscillations High energy (E ≳ 5 Me. V) MSW conversion Yusuke Koshio Neutrino 2014 Energy [Me. V] Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Neutrinos are Brighter at Night Super-Kamiokande Collaboration ar. Xiv: 1312. 5176 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Models Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Equations of Stellar Structure Assume spherical symmetry and static structure (neglect kinetic energy) Excludes: Rotation, convection, magnetic fields, supernova-dynamics, … Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Constructing a Solar Model: Fixed Inputs Solve stellar structure equations with good microphysics, starting from a zero-age main-sequence model (chemically homogeneous) to present age Fixed quantities Mass M⊙ = 1. 989 1033 g 0. 1% Age t⊙ = 4. 57 109 yrs 0. 5% Kepler’s 3 rd law Meteorites Quantities to match Luminosity Radius Metals/hydrogen ratio L⊙ = 3. 842 1033 erg s-1 0. 4% Solar constant R⊙ = 6. 9598 1010 cm 0. 1% Angular diameter (Z/X)⊙ = 0. 0229 Photosphere and meteorites Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Constructing a Solar Model: Free Parameters 3 free parameters • Convection theory has 1 free parameter: Mixing length parameter a. MLT determines the temperature stratification where convection is not adiabatic (upper layers of solar envelope) • 2 of 3 quantities determining the initial composition: Xini, Yini, Zini (linked by Xini + Yini + Zini = 1). Individual elements grouped in Zini have relative abundances given by solar abundance measurements (e. g. GS 98, AGS 05) • Construct 1 M⊙ initial model with Xini, Zini, Yini = 1 - Xini - Zini and a. MLT • Evolve for the solar age t⊙ • Match (Z/X)⊙, L⊙ and R⊙ to better than 10 -5 Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Standard Solar Model Output Information Eight neutrino fluxes: Production profiles and integrated values Chemical profiles X(r), Y(r), Zi(r) electron and neutron density profiles Thermodynamic quantities as a function of radius: T, P, density r, sound speed c Surface helium abundance Ysurf (Z/X and 1 = X + Y + Z leave 1 degree of freedom) Depth of the convective envelope RCZ Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Standard Solar Model: Internal Structure Temperature Mass density 14 N Hydrogen Helium 12 C Convection RCZ Georg Raffelt, MPI Physics, Munich Convection 13 C Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Models Helioseismology and the New Opacity Problem Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Helioseismology: Sun as a Pulsating Star Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Helioseismology: p-Modes Credit: Jørgen Christensen-Dalsgaard Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Examples for Solar Oscillations + + = http: //astro. phys. au. dk/helio_outreach/english/ Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Helioseismology: Observations • Doppler observations of spectral lines measure velocities of a few cm/s • Differences in the frequencies of order m. Hz • Very long observations needed. Bi. SON network (low-l modes) has data for 5000 days • Relative accuracy in frequencies is 10 -5 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Helioseismology: Comparison with Solar Models • Oscillation frequencies depend on r, P, g, c • Inversion problem: From measured frequencies and from a reference solar model determine solar structure • Output of inversion procedure: dc 2(r), dr(r), RCZ, YSURF Relative sound-speed difference between helioseismological model and standard solar model Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

New Solar Opacities (Asplund, et al. 2005, 2009) • Large change in solar composition: Mostly reduction in C, N, O, Ne • Results presented in many papers by the “Asplund group” • Summarized in Asplund, Grevesse, Sauval & Scott (2009) Authors (Z/X)⊙ Main changes (dex) Grevesse 1984 0. 0277 Anders & Grevesse 1989 0. 0267 Grevesse & Noels 1993 0. 0245 Grevesse & Sauval 1998 0. 0229 DC = -0. 04, DN = -0. 07, DO = -0. 1 Asplund, Grevesse & Sauval 2005 0. 0165 DC = -0. 13, DN = -0. 14, DO = -0. 17 DNe = -0. 24, DSi = -0. 05 Asplund, Grevesse, Sauval & Scott (ar. Xiv: 0909. 0948, 2009 ) Scott ( 0. 0178 DC = -0. 1, DN = +0. 06 Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Origin of Changes Spectral lines from solar photosphere and corona • Improved modeling 3 D model atmospheres MHD equations solved NLTE effects accounted for in most cases • Improved data Better selection of spectral lines Previous sets had blended lines (e. g. oxygen line blended with nickel line) • Volatile elements do not aggregate easily into solid bodies e. g. C, N, O, Ne, Ar only in solar spectrum Meteorites • Refractory elements e. g. Mg, Si, S, Fe, Ni both in solar spectrum and meteorites meteoritic measurements more robust Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Consequences of New Element Abundances • Much improved modeling What is good • Different lines of same element give same abundance (e. g. CO and CH lines) • Sun has now similar composition to solar neighborhood • Agreement between helioseismology New problems and SSM very much degraded • Was previous agreement a coincidence? Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Standard Solar Model 2005: Old and New Opacity Sound Speed Density Old: BS 05 (GS 98) New: BS 05 (ASG 05) Helioseismology RCZ 0. 713 0. 728 0. 713 ± 0. 001 YSURF 0. 243 0. 229 0. 2485 ± 0. 0035 <dc> 0. 001 0. 005 — <dr> 0. 012 0. 044 — Neutrinos. Summer in Astrophysics Cosmology, Georg Raffelt, MPI Physics, Munich Adapted from A. Serenelli’s lectures at Scottish Universities School and in Physics 2006 NBI, 23– 27 June 2014

Old and New Neutrino Fluxes Old: (GS 98) New: (AGSS 09) Best Measurements Flux cm-2 s-1 Error % pp 5. 98 1010 0. 6 6. 03 1010 0. 6 6. 05 1010 0. 6 pep 1. 44 108 1. 1 1. 47 108 1. 2 1. 46 108 1. 2 hep 8. 04 103 30 8. 31 103 30 18 103 45 7 Be 5. 00 109 7 4. 56 109 7 4. 82 109 4. 5 8 B 5. 58 106 14 4. 59 106 14 5. 0 106 3 13 N 2. 96 108 14 2. 17 108 14 < 6. 7 108 15 O 2. 23 108 15 1. 56 108 15 < 3. 2 108 17 F 5. 52 106 17 3. 40 106 16 < 59 106 • Directly measured 7 -Be (Borexino) and 8 -B (SNO) fluxes are halfway between models • CN fluxes depend linearly on abundances, measurements needed Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Prospect for CNO Flux Measurements CNO neutrino measurements require excellent background reduction/subtraction Not achievable in Borexino in near future. Perhaps in SNO+ ? Borexino Collaboration, ar. Xiv: 1308. 0443 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Models Particle Bounds Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Neutrino Limit on Solar Energy Losses Self-consistent models of the present-day Sun provide a simple power-law connection between a new energy loss La (e. g. axions) and the all-flavor solar neutrino flux from the B 8 reaction as measured by SNO Gondolo & Raffelt, ar. Xiv: 0807. 2926 Schlattl, Weiss & Raffelt, hep-ph/9807476 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Hidden Photons (HPs) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Hidden Photon Constraints (old) (new) Nominal limit Redondo & Raffelt, ar. Xiv: 1305. 2920 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Summary of Hidden Photon Limits Redondo & Raffelt, ar. Xiv: 1305. 2920 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Solar Models Search for Solar Axions Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Axion Physics in a Nut Shell Particle-Physics Motivation CP conservation in QCD by Peccei-Quinn mechanism p 0 Axions a ~ mpfp mafa g Axions thermally produced in stars, e. g. by Primakoff production g a a For fa ≫ fp axions are “invisible” and very light Cosmology In spite of small mass, axions are born non-relativistically (non-thermal relics) Cold dark matter candidate ma ~ 10 me. V or even smaller Georg Raffelt, MPI Physics, Munich Solar and Stellar Axions g • Limits from avoiding excessive energy drain • Solar axion searches (CAST, Sumico) Search for Axion Dark Matter Microwave resonator (1 GHz = 4 me. V) N a Primakoff conversion g Bext S ADMX-LF (UW Seattle) ADMX-HF (Yale) Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Experimental Tests of Invisible Axions Pierre Sikivie: Macroscopic B-field can provide a large coherent transition rate over a big volume (low-mass axions) • Axion helioscope: Look at the Sun through a dipole magnet • Axion haloscope: Look for dark-matter axions with A microwave resonant cavity Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Search for Solar Axions Axion Helioscope (Sikivie 1983) Primakoff production a g Sun Axion flux a N g Magnet S Axion-Photon-Oscillation Ø Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008) Ø CERN Axion Solar Telescope (CAST) (Data since 2003) Alternative technique: Bragg conversion in crystal Experimental limits on solar axion flux from dark-matter experiments (SOLAX, COSME, DAMA, CDMS. . . ) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Axion-Photon-Transitions as Particle Oscillations Raffelt & Stodolsky, PRD 37 (1988) 1237 Photon refractive and birefringence effects (Faraday rotation, Cotton-Mouton-effect) Stationary Klein-Gordon equation for coupled a-g-system Axion-photon transitions • Axions roughly like another photon polarization state • In a homogeneous or slowly varying B-field, a photon beam develops a coherent axion component Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

CERN Axion Solar Telescope (CAST) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Extending to higher mass values with gas filling Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Helioscope Limits First experimental crossing of the KSVZ line CAST-I results: PRL 94: 121301 (2005) and JCAP 0704 (2007) 010 CAST-II results (He-4 filling): JCAP 0902 (2009) 008 CAST-II results (He-3 filling): PRL 107: 261302 (2011) and in preparation (2013) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Next Generation Axion Helioscope (IAXO) at CERN • Irastorza et al. : Towards a new generation axion helioscope, ar. Xiv: 1103. 5334 • Armengaud et al. : Conceptual Design of the International Axion Observatory (IAXO), ar. Xiv: 1401. 3233 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Geo Neutrinos Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

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 Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Geo Neutrino Spectrum 40 K 232 Th 238 U Bellini, Ianni, Ludhova, Mantovani & Mc. Donough, ar. Xiv: 1310. 3732 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Extreme Geo Neutrino Fluxes Schematic radioactive element distribution for fixed heat flux Minimal neutrino flux at detector Maximal neutrino flux at detector Bellini, Ianni, Ludhova, Mantovani & Mc. Donough, ar. Xiv: 1310. 3732 Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Geo Neutrinos Expected Geoneutrino Flux Kam. LAND Scintillator-Detector (1000 t) Reactor Background Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Kam. LAND Geo-Neutrino Flux Beginning of neutrino geophysics! Kam. LAND Collaboration, ar. Xiv: 1303. 4667 (2013) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Reactor On-Off Kam. LAND Data 2011 Earthquake Reactors shut down Scintillator Purification Kam. LAND-Zen Construction Kam. LAND Collaboration, ar. Xiv: 1303. 4667 (2013) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014

Applied Anti-Neutrino Physics (AAP) Annual Conference Series since 2004 • Neutrino geophysics • Reactor monitoring (“Neutrinos for Peace”) • Relatively small detectors can measure nuclear activity without intrusion • Of interest for monitoring by International Atomic Energy Agency (Monitors fissile material in civil nuclear cycles) Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23– 27 June 2014