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.

Slides:

Advertisements

Similar presentations

Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 16 Our Star, the Sun CHAPTER 16 Our Star, the Sun.

Advertisements

Standard Solar Model Calculation of Neutrino Fluxes Aldo Serenelli Institute for Advanced Study NOW 2006 Conca Specchiulla 11-Sept-2006.

SUSSP61: Neutrino Physics - St. Andrews, Scotland – 8 th to 23 rd, August, 2006 Standard Solar Models II Aldo Serenelli Institute for Advanced Study, Princeton.

The Standard Solar Model and Its Evolution Marc Pinsonneault Ohio State University Collaborators: Larry Capuder Scott Gaudi.

Einstein’s Energy Mass Equivalence Powers the Sun!

Neutrino oscillations/mixing

Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%

Solar Physics and Sun-Earth Connection ( introduction ) Samuel Danagoulian NC A&T State University Teacher’s Workshop,

Slide 1 Test 2 results Test 2 average: 77 (test 1: 82) Test 2 median: 79 (test 1: 87)

Properties of stars during hydrogen burning Hydrogen burning is first major hydrostatic burning phase of a star: Hydrostatic equilibrium: a fluid element.

1 B.Ricci* What have we learnt about the Sun from the measurement of 8B neutrino flux? Experimental results SSM predictions SSM uncertainties on  (8B)

The Sun The Sun in X-rays over several years The Sun is a star: a shining ball of gas powered by nuclear fusion. Luminosity of Sun = 4 x erg/s =

© 2005 Pearson Education Inc., publishing as Addison-Wesley The Sun: Our Star 29 April 2008.

Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%

Physics 681: Solar Physics and Instrumentation – Lecture 5 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.

© 2005 Pearson Education Inc., publishing as Addison-Wesley The Sun: Our Star Lecture 21 How does the Sun work ? What is the energy source for the Sun.

Question 1 1) core 2) corona 3) photosphere 4) chromosphere 5) convection zone The visible light we see from our Sun comes from which part?

Zachary Robinson Phys 406.  What creates the sun’s energy? ◦ Composition of Sun ◦ Fusion in the Sun (and other stars)  Creation of the elements  Studying.

SUSSP61: Neutrino Physics - St

李玉峰中科院高能所 JUNO中微子天文和天体物理学研讨会

The Sun as a Star The “Surface” of the Sun and Its Structure Outer Layers – 3 distinct region Photosphere Chromosphere Corona.

Solar Neutrinos Dr Robert Smith Astronomy Centre University of Sussex.

The Interior of Stars III

The Sun Internal structure of the Sun Nuclear fusion –Protons, neutrons, electrons, neutrinos –Fusion reactions –Lifetime of the Sun Transport of energy.

The Elementary Particles. e−e− e−e− γγ u u γ d d The Basic Interactions of Particles g u, d W+W+ u d Z0Z0 ν ν Z0Z0 e−e− e−e− Z0Z0 e−e− νeνe W+W+ Electromagnetic.

Limits on Solar CNO From Session 13 IAU - XXVIII GA Aldo Serenelli Institute of Space Sciences (CSIC-IEEC) Bellaterra, Spain Beijing.

Lecture 13. Review: Static Stellar structure equations Hydrostatic equilibrium: Mass conservation: Equation of state: Energy generation: Radiation Convection.

PHYS 1621 The Sun Some Properties Diameter times Earth’s Volume - about 1,000,000 times Earth’s Mass - about 300,000 times Earth’s 99.8% of Solar.

Solar Energy p-p chain is source of Solar Energy Sun could last 1.

Lecture 2: Formation of the chemical elements Bengt Gustafsson: Current problems in Astrophysics Ångström Laboratory, Spring 2010.

Methods and problems in low energy neutrino experiments (solar, reactors, geo-) I G. Ranucci ISAPP 2011 International School on Astroparticle physics THE.

Astronomy 100 – Section 2 As Presented by Paul Ricker This class: The Sun II: Interior.

The Standard Solar Model and Experiments Predictions versus experiments Uncertainties in predictions Challenges and open questions BP00: astro-ph/

Wednesday, Feb. 14, 2007PHYS 5326, Spring 2007 Jae Yu 1 PHYS 5326 – Lecture #6 Wednesday, Feb. 14, 2007 Dr. Jae Yu 1.Neutrino Oscillation Formalism 2.Neutrino.

The Sun: Part 2. Temperature at surface = 5800 K => yellow (Wien’s Law) Temperature at center = 15,000,000 K Average density = 1.4 g/cm 3 Density at center.

SNO and the new SNOLAB SNO: Heavy Water Phase Complete Status of SNOLAB Future experiments at SNOLAB: (Dark Matter, Double beta, Solar, geo-, supernova.

Kopylov A.V. Erice School/Workshop 2009 on Neutrinos in Cosmology, in Astro, in Particle and in Nuclear Physics in Erice/Trapani/Sicily/Italy on September.

Lesson 13 Nuclear Astrophysics. Elemental and Isotopic Abundances.

What temperature would provide a mean kinetic energy of 0.5 MeV? By comparison, the temperature of the surface of the sun  6000 K.

Dr Matt Burleigh The Sun and the Stars. Dr Matt Burleigh The Sun and the Stars The Hertzsprung-Russell Diagram (E. Hertzsprung and H.N. Russell) Plot.

J. Goodman – January 03 The Solution to the Solar Problem Jordan A. Goodman University of Maryland January 2003 Solar Neutrinos MSW Oscillations Super-K.

Neutrinos: What we’ve learned and what we still want to find out Jessica Clayton Astronomy Club November 10, 2008.

PHYS 1621 Proton-proton cycle 3 steps. PHYS 1622 Layers of the Sun Mostly Hydrogen with about 25% Helium. Small amounts of heavier elements Gas described.

Masatoshi Koshiba Raymond Davis Jr. The Nobel Prize in Physics 2002 "for pioneering contributions to astrophysics, in particular for the detection of cosmic.

Cosmological mass bounds on hot-dark matter axions Alessandro MIRIZZI (MPI, Munich) NOW Neutrino Oscillation Workshop Conca Specchiulla, September.

A Brief Review of “Matter”. Atom nucleus electron e-e- (proton,neutrons) p+p+ n ● 10,000,000 atoms can fit across a period in your textbook. ● The nucleus.

The Sun: Part 2. Temperature at surface = 5800 K => yellow (Wien’s Law) Temperature at center = 15,000,000 K Average density = 1.4 g/cm 3 Density at center.

Announcements Grades for the first hour exam should be available on WebCT on Tuesday. Observing during this week will count for extra credit on the first.

INT Solar models Composition, neutrinos & accretion Aldo Serenelli (MPA)

Results and perspectives of the solar axion search with the CAST experiment Esther Ferrer Ribas IRFU/CEA-Saclay For the CAST Collaboration Rencontres de.

Chapter 10 Our Star.

Main Sequence Stars Internal structure Nuclear fusion –Protons, neutrons, electrons, neutrinos –Fusion reactions –Lifetime of the Sun Transport of energy.

P Spring 2002 L18Richard Kass The Solar Neutrino Problem M&S Since 1968 R.Davis and collaborators have been measuring the cross section of:

Solar Neutrinos By Wendi Wampler. What are Neutrinos? Neutrinos are chargeless, nearly massless particles Neutrinos are chargeless, nearly massless particles.

Universe Tenth Edition Chapter 16 Our Star, the Sun Roger Freedman Robert Geller William Kaufmann III.

Georg Raffelt, MPI Physics, Munich IAXO Workshop, INFN Frascati, 18–19 April 2016 Axion Landscape Solar Axions Supernova 1987A Dark Matter Long-Range Force.

STELLAR EVOLUTION – THE STANDARD SOLAR MODEL AND SOLAR NEUTRINOS – MARIE ZECH.

Solar Neutrinos Learning about the core of the Sun Guest lecture: Dr. Jeffrey Morgenthaler Jan 26, 2006.

Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23–27 June 2014 Crab NebulaNeutrinos in Astrophysics and Cosmology Introductory.

Solar neutrino physics The core of the Sun reaches temperatures of  15.5 million K. At these temperatures, nuclear fusion can occur which transforms 4.

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

Our Star, the Sun Chapter Eighteen. Guiding Questions 1.What is the source of the Sun’s energy? 2.What is the internal structure of the Sun? 3.How can.

X-ray telescope: D. Greenwald, R. Kotthaus, G. Lutz

G. Dattoli and F. Nguyen ENEA-FRASCATI

© 2017 Pearson Education, Inc.

Solar Neutrino Problem

The Sun Internal structure of the Sun Nuclear fusion

Pauli´s new particle * nt nm ne e m t Beta-Decay Pa 234 b (electron)

7. Internal structure. II.

1930: Energy conservation violated in β-decay

Presentation transcript:

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

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)

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

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

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 – 2006

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

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 / Atoms) Theoretical Prediction 6  9 SNU “Solar Neutrino Problem” since 1968 Results of Chlorine Experiment (Homestake) ApJ 496:505, 1998 Average Rate

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

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)

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

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)

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

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

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

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

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)

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

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 

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/ )

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

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

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)

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

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

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: (25 May 2008)

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

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

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

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

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

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

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

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

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, …

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

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 ⊙ =  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 ⊙ =  erg s % Solar constant Solar radius R ⊙ =  cm 0.1% Angular diameter Solar metals/hydrogen ratio (Z/X) ⊙ = Photosphere and meteorites

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

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

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

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

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

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

Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Examples for Solar Oscillations ++ =

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

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

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

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 Anders & Grevesse  C = -0.1,  N = Grevesse & Noels Grevesse & Sauval  C = -0.04,  N = -0.07,  O = -0.1 Asplund, Grevesse & Sauval  C = -0.13,  N = -0.14,  O =  Ne = -0.24,  Si = Asplund, Grevesse, Sauval & Scott () Asplund, Grevesse, Sauval & Scott (arXiv: , 2009) Adapted from A. Serenelli’s lectures at Scottish Universities Summer School in Physics 2006

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

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

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 ± Y SURF ± — —

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       0.6 pep pep 1.44  10 8   10 8   10 8  1.2 hep hep 8.04  10 3   10 3  3018  10 3  45 7 Be 7 Be 5.00  10 9 777  10 9 777  10 9  4.5 8B8B8B8B 5.58  10 6   10 6   10 6 3333 13 N 2.96  10 8   10 8  14< 6.7  O 2.23  10 8   10 8  15< 3.2  F 5.52  10 6   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

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

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

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

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)

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

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...)

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

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

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

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

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

Georg Raffelt, MPI Physics, Munich ISAPP 2011, 3/8/11, Varenna, Italy Helioscope Limits CAST-I results: PRL 94: (2005) and JCAP 0704 (2007) 010 CAST-II results (He-4 filling): JCAP 0902 (2009) 008 CAST-II results (He-3 filling): arXiv: First experimental crossing of the KSVZ line Solar neutrino limit

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/ Gondolo & Raffelt, arXiv:

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:

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