1. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Neutrinos from the Sun Neutrinos and the Stars II Neutrinos from the Sun Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany ISAPP 2011, International School on Astroparticle Physics 26 th July–5 th August 2011, Varenna, Italy

2. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Neutrinos from the SunReaction-chains Energy 26.7 MeV Helium Solar radiation: 98 % light 2 % neutrinos 2 % neutrinos At Earth 66 billion neutrinos/cm 2 sec Hans Bethe (1906  2005, Nobel prize 1967) Thermonuclear reaction chains (1938)

3. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Hydrogen Burning: Proton-Proton Chains < 0.420 MeV 1.442 MeV PP-I < 18.8 MeV hep 0.862 MeV0.384 MeV < 15 MeV PP-IIPP-III 15%85% 0.02%90%10% 0.24%100%

4. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Neutrino Spectrum

5. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Proposing the First Solar Neutrino Experiment John Bahcall 1934 – 2005 Raymond Davis Jr. 1914 – 2006

6. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy First Measurement of Solar Neutrinos 600 tons of Perchloroethylene Homestake solar neutrino observatory (1967–2002) Inverse beta decay of chlorine

7. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Average (1970  1994) 2.56  0.16 stat  0.16 sys SNU (SNU = Solar Neutrino Unit = 1 Absorption / sec / 10 36 Atoms) Theoretical Prediction 6  9 SNU “Solar Neutrino Problem” since 1968 Results of Chlorine Experiment (Homestake) ApJ 496:505, 1998 Average Rate

8. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Neutrino Flavor Oscillations Bruno Pontecorvo (1913–1993) Invented nu oscillations Two-flavor mixing Oscillation Length z

9. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy GALLEX/GNO and SAGE Inverse Beta Decay Gallium  Germanium GALLEX/GNO (1991–2003)

10. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Gallium Results as Shown at Neutrino 2006

11. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Cherenkov Effect Water Elastic scattering or CC reaction Neutrino Light Cherenkov Ring Electron or Muon (Charged Particle)

12. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Super-Kamiokande Neutrino Detector (Since 1996) 42 m 39.3 m

13. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Super-Kamiokande: Sun in the Light of Neutrinos

14. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Sudbury Neutrino Observatory (SNO) 1000 tons of heavy water

15. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Sudbury Neutrino Observatory (SNO) 1000 tons of heavy water

16. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Sudbury Neutrino Observatory (SNO) 1000 tons of heavy water Normal (light) water H 2 0 Heavy water D 2 0 Nucleus of hydrogen (proton) Nucleus of heavy hydrogen (deuterium)

17. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Sudbury Neutrino Observatory (SNO) Heavy hydrogen (deuterium) Electron neutrinos Heavy hydrogen (deuterium) All neutrino flavors

18. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Missing Neutrinos from the Sun Homestake 7 Be 8B8B CNO Chlorine Gallex/GNO SAGE CNO 7 Be pp 8B8B Gallium Electron-Neutrino Detectors (Super-) Kamiokande 8B8B Water e + e   e + e  SNO 8B8B e + d  p + p + e  Heavy Water 8B8B + d  p + n + Heavy Water All Flavors SNO 8B8B Water + e   + e 

19. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Charged and Neutral-Current SNO Measurements Ahmad et al. (SNO Collaboration), PRL 89:011301,2002 (nucl-ex/0204008)

20. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Final SNO Measurement of Boron-8 Flux SNO Collaboration, arXiv:0910.2984

21. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy KamLAND Long-Baseline Reactor-Neutrino Experiment

22. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Oscillation of Reactor Neutrinos at KamLAND (Japan) Oscillation pattern for anti-electron neutrinos from Japanese power reactors as a function of L/E KamLAND Scintillator detector (1000 t)

23. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Best-fit “solar” oscillation parameters

24. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Neutrino Spectrum 7-Be line measured by Borexino (2007)

25. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Neutrino Spectroscopy with BOREXINO 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 arXiv:0805.3843 (25 May 2008)

26. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Neutrinos in Borexino Borexino Collaboration, arXiv:1104.1816

27. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Geo Neutrinos

28. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy 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

29. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Geo Neutrinos Expected Geoneutrino Flux Reactor Background KamLAND Scintillator-Detector (1000 t)

30. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Latest KamLAND Measurements of Geo Neutrinos K. Inoue at Neutrino 2010

31. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Geo Neutrinos in Borexino Borexino Collaboration, arXiv:1003.0284v Geo neutrino signal

32. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Geo Neutrinos in Borexino Borexino Collaboration, arXiv:1003.0284 Expectation Reactors Expectation BSE model of Earth 68% 95% 99.73%

33. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Models

34. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Equations of Stellar Structure Assume spherical symmetry and static structure (neglect kinetic energy) Excludes: Rotation, convection, magnetic fields, supernova-dynamics, …

35. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Convection in Main-Sequence Stars Kippenhahn & Weigert, Stellar Structure and Evolution Sun

36. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Constructing a Solar Model: Fixed Inputs Solve stellar structure equations with good microphysics, starting from a zero-age main-sequence model (chemically homogeneous star) to present age Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006 Fixed quantities Solar mass M ⊙ = 1.989  10 33 g 0.1% Kepler’s 3 rd law Solar age t ⊙ = 4.57  10 9 yrs 0.5% Meteorites Quantities to match Solar luminosity L ⊙ = 3.842  10 33 erg s -1 0.4% Solar constant Solar radius R ⊙ = 6.9598  10 10 cm 0.1% Angular diameter Solar metals/hydrogen ratio (Z/X) ⊙ = 0.0229Photosphere and meteorites

37. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy 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 the 3 quantities determining the initial composition: X ini, Y ini, Z ini (linked by X ini + Y ini + Z ini = 1). Individual elements grouped in Z ini have relative abundances given by solar abundance measurements (e.g. GS98, AGSS09) Construct a 1 M ⊙ initial model with X ini, Z ini, Y ini = 1  X ini  Z ini and a MLT Evolve it for the solar age t ⊙ Match (Z/X) ⊙, L ⊙ and R ⊙ to better than one part in 10 5 Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006

38. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Standard Solar Model Output Information Eight neutrino fluxes: Production profiles and integrated values. Only 8 B flux directly measured (SNO) Chemical profiles X(r), Y(r), Z i (r)  electron and neutron density profiles (needed for matter effects in neutrino studies) Thermodynamic quantities as a function of radius: T, P, density (  ), sound speed (c) Surface helium abundance Y surf (Z/X and 1 = X + Y + Z leave 1 degree of freedom) Depth of the convective envelope, R CZ Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006

39. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Standard Solar Model: Internal Structure

40. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Models Helioseismology and the New Opacity Problem New Opacity Problem

41. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Helioseismology: Sun as a Pulsating Star Discovery of oscillations: Leighton et al. (1962) Sun oscillates in > 10 5 eigenmodes Frequencies of order mHz (5-min oscillations) Individual modes characterized by radial n, angular l and longitudinal m numbers Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006

42. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Helioseismology: p-Modes Solar oscillations are acoustic waves (p-modes, pressure is the restoring force) stochastically excited by convective motions Outer turning-point located close to temperature inversion layer Inner turning-point varies, strongly depends on l (centrifugal barrier) Credit: Jørgen Christensen-Dalsgaard

43. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Examples for Solar Oscillations http://astro.phys.au.dk/helio_outreach/english/ ++ =

44. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Helioseismology: Observations Doppler observations of spectral lines measure velocities of a few cm/s Differences in the frequencies of order mHz Very long observations needed. BiSON network (low-l modes) has data for  5000 days Relative accuracy in frequencies is 10  5

45. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Full-Disk Dopplergram of the Sun

46. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Helioseismology: Comparison with Solar Models Oscillation frequencies depend on , P, g, c Inversion problem: From measured frequencies and from a reference solar model determine solar structure Output of inversion procedure:  c 2 (r),  (r), R CZ, Y SURF Relative sound-speed difference between helioseismological model and standard solar model

47. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy 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 19840.0277 Anders & Grevesse 19890.0267  C = -0.1,  N = +0.06 Grevesse & Noels 19930.0245 Grevesse & Sauval 1998 0.0229  C = -0.04,  N = -0.07,  O = -0.1 Asplund, Grevesse & Sauval 20050.0165  C = -0.13,  N = -0.14,  O = -0.17  Ne = -0.24,  Si = -0.05 Asplund, Grevesse, Sauval & Scott () Asplund, Grevesse, Sauval & Scott (arXiv:0909.0948, 2009)0.0178 Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006

48. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Origin of Changes Improved modeling 3D 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) Spectral lines from solar photosphere and corona Meteorites Volatile elements do not aggregate easily into solid bodies e.g. C, N, O, Ne, Ar only in solar spectrum Refractory elements e.g. Mg, Si, S, Fe, Ni both in solar spectrum and meteorites meteoritic measurements more robust

49. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Consequences of New Element Abundances Much improved modeling Different lines of same element give same abundance (e.g. CO and CH lines) Sun has now similar composition to solar neighborhood What is good New problems Agreement between helioseismology and SSM very much degraded Was previous agreement a coincidence? Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006

50. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Standard Solar Model 2005: Old and New Opacity Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006 Sound SpeedDensity Old: BS05 (GS98)New: BS05 (ASG05)Helioseismology R CZ 0.7130.7280.713 ± 0.001 Y SURF 0.2430.2290.2485 ± 0.0035 0.0010.005— 0.0120.044—

51. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Old and New Neutrino Fluxes Old: (GS98) New: (AGSS09) Best Measurements Flux cm -2 s -1 Error % Flux cm -2 s -1 Error % Flux cm -2 s -1 Error % pp pp 5.98  10 10  0.66.03  10 10  0.66.05  10 10  0.6 pep pep 1.44  10 8  1.11.47  10 8  1.21.46  10 8  1.2 hep hep 8.04  10 3  308.31  10 3  3018  10 3  45 7 Be 7 Be 5.00  10 9 7777 4.56  10 9 7777 4.82  10 9  4.5 8B8B8B8B 5.58  10 6  14 4.59  10 6  14 5.0  10 6 3333 13 N 2.96  10 8  142.17  10 8  14< 6.7  10 8 15 O 2.23  10 8  151.56  10 8  15< 3.2  10 8 17 F 5.52  10 6  173.40  10 6  16< 59  10 6 Directly measured 7-Be (Borexino) and 8-B (SNO) fluxes are halfway between CN fluxes depend linearly on abundances, measurements needed

52. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Hydrogen Burning: CNO Cycle

53. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Neutrino Spectrum Including CNO Reactions

54. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Solar Models Search for Solar Axions

55. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Axion Physics in a Nut Shell CP conservation in QCD by Peccei-Quinn mechanism For f a ≫ f  axions are “invisible” and very light  Axions a ~  0 m  f   m a f a   a Particle-Physics Motivation Axions thermally produced in stars, e.g. by Primakoff production Limits from avoiding excessive energy drain Solar axion searches (CAST, Sumico) a  Solar and Stellar Axions In spite of small mass, axions are born non-relativistically (non-thermal relics) Cold dark matter candidate m a ~ 10  eV or even smaller CosmologySearch for Axion Dark Matter S N  a B ext Microwave resonator (1 GHz = 4  eV) Primakoff conversion ADMX (Seattle) New CARRACK (Kyoto)

56. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy 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

57. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Search for Solar Axions  a Sun Primakoff production Axion Helioscope (Sikivie 1983)  Magnet S N a Axion-Photon-Oscillation  Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008)  CERN Axion Solar Telescope (CAST) (Data since 2003) Axion flux Alternative technique: Bragg conversion in crystal Experimental limits on solar axion flux from dark-matter experiments (SOLAX, COSME, DAMA, CDMS...)

58. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Axion-Photon-Transitions as Particle Oscillations Stationary Klein-Gordon equation for coupled a-  -system Axions roughly like another photon polarization state In a homogeneous or slowly varying B-field, a photon beam develops a coherent axion component Raffelt & Stodolsky, PRD 37 (1988) 1237 Photon refractive and birefringence effects (Faraday rotation, Cotton-Mouton-effect) Axion-photon transitions

59. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Tokyo Axion Helioscope (“Sumico”) Moriyama, Minowa, Namba, Inoue, Takasu & Yamamoto PLB 434 (1998) 147 Inoue, Akimoto, Ohta, Mizumoto, Yamamoto & Minowa PLB 668 (2008) 93

60. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy LHC Magnet Mounted as a Telescope to Follow the Sun

61. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy CAST at CERN

62. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Extending to higher mass values with gas filling

63. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Helioscope Limits 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): arXiv:1106.3919 First experimental crossing of the KSVZ line Solar neutrino limit

64. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy 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 L a (e.g. axions) and the all-flavor solar neutrino flux from the B8 reaction as measured by SNO Schlattl, Weiss & Raffelt, hep-ph/9807476 Gondolo & Raffelt, arXiv:0807.2926

65. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Next Generation Axion Helioscope I. Irastorza et al., “Towards a new generation axion helioscope”, arXiv:1103.5334

66. Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Helioscope Prospects SN 1987A Limits