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Axions. Georg Raffelt Max Planck Institute for Physics Munich. xions. Theoretical Motivation Cosmological Role Experimental Searches. Axion Physics in a Nut Shell. Particle-Physics Motivation. Solar and Stellar Axions. CP conservation in QCD by Peccei-Quinn mechanism. - PowerPoint PPT Presentation
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Do White Dwarfs Need Axion Cooling?
Axions
Theoretical MotivationCosmological RoleExperimental SearchesGeorg RaffeltMax Planck Institute for PhysicsMunich
xionsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Physics in a Nut ShellCP conservation in QCD byPeccei-Quinn mechanismFor fa fp axions are invisibleand very light Axions a ~ p0 mpfp mafagga
Particle-Physics Motivation Axions thermally produced in stars, e.g. by Primakoff production
Limits from avoiding excessive energy drain Solar axion searches (CAST, Sumico) agSolar and Stellar Axions In spite of small mass, axions are born non-relativistically (non-thermal relics) Cold dark matter candidate ma ~ 10 meV or even smallerCosmology
Search for Axion Dark MatterSNgaBext Microwave resonator (1 GHz = 4 meV)Primakoffconversion ADMX (Seattle) New CARRACK (Kyoto)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions
xionsParticle-Physics OriginsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 CP Violation in Particle Physics
Physics Nobel Prize 2008Discrete symmetries in particle physics
C Charge conjugation, transforms particles to antiparticles violated by weak interactions
P Parity, changes left-handedness to right-handedness violated by weak interactions
T Time reversal, changes direction of motion (forward to backward)
CPT exactly conserved in quantum field theory
CP conserved by all gauge interactions violated by three-flavor quark mixing matrixM. KobayashiT. MaskawaAll measured CP-violating effects derive from a single phase in the quark mass matrix (Kobayashi-Maskawa phase), i.e. from complex Yukawa couplings
Cosmic matter-antimatter asymmetry requires new ingredientsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Cabbibo-Kobayashi-Maskawa (CKM) MatrixQuark interaction with W boson(charged-current electroweak interaction) Unitary Cabbibo-Kobayashi-Maskawa matrixrelates mass eigenstatesto weak interaction eigenstates
VCKM depends on three mixing angles and one phase d,explaining all observed CP-violation
Precision tests use unitarity triangles consisting of products of measuredcomponents of VCKM, for example:
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Measurements of CKM Unitarity Triangle
CKMfitter Grouphttp://ckmfitter.in2p3.frUTfit Collaborationhttp://www.utfit.orgGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Kobayashi and Maskawa
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 The CP Problem of Strong InteractionsReal quarkmassPhase fromYukawa couplingAnglevariableRemove phase of mass term by chiral transformation of quark fieldsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Neutron Electric Dipole Moment
Violates time reversal (T) andspace reflection (P) symmetriesNatural scaleExperimental limitLimit on coefficientGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Strong CP Problem
EquivalentEquivalentGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Dynamical SolutionPeccei & Quinn 1977, Wilczek 1978, Weinberg 1978CP-symmetry dynamicallyrestoredGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 The Pool Table Analogy (Pierre Sikivie 1996)GravitySymmetricrelativeto gravityPool tableNew degree of freedom Axion(Weinberg 1978, Wilczek 1978)AxisSymmetrydynamicallyrestored (Peccei & Quinn 1977)SymmetrybrokenFloor inclinedfaGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 33 Years of Axions
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 The Cleansing Axion
Frank WilczekI named them after a laundry detergent, since they clean up a problem with an axial current. (Nobel lecture 2004)
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion as a Nambu-Goldstone Boson
Periodic variable (angle)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 From Standard to Invisible AxionsStandard ModelStandard Axion
Weinberg 1978, Wilczek 1978Invisible Axion
Kim 1979, Shifman,Vainshtein, Zakharov 1980,Dine, Fischler, Srednicki 1981Zhitnitsky 1980 All Higgs degrees of freedom are used up Peccei-Quinn scale fa = fEW (electroweak scale)
Two Higgs fields, separately giving mass to up-type quarks and down-type quarks Additional Higgs with fa fEW
Axions very light and and very weakly interacting
No room for Peccei-Quinn symmetry and axionsStandard axions quicklyruled out experimentally New scale required
Axions can be cold dark matter
Can be detectedGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Simplest Invisible Axion: KSVZ Model
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Properties Mass (generic) Nucleon coupling (axial vector) Electron coupling (optional) Gluon coupling (generic) Photon coupling Pion couplingNNa
eea
aGG
gga
apppGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions
xionsAstrophysical BoundsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Emission Processes in StarsElectronsNucleonsPhotonsNucleonBremsstrahlungPrimakoffComptonPairAnnihilationElectromagneticBremsstrahlung
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Supernova 1987A Energy-Loss Argument
SN 1987A neutrino signalLate-time signal most sensitive observableEmission of very weakly interactingparticles would steal energy from theneutrino burst and shorten it.(Early neutrino burst powered by accretion, not sensitive to volume energy loss.) Neutrino diffusionNeutrinosphere Volume emission of new particlesGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Diffuse Supernova Axion Background (DSAB)
Raffelt, Redondo & Viauxwork in progress (2011) Neutrinos from all core-collapse SNe comparable to photons from all stars
Diffuse Supernova Neutrino Background (DSNB) similar energy density as extra-galactic background light (EBL), approx 10% of CMB energy density
DSNB probably next astro neutrinos to be measuredGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Do White Dwarfs Need Axion Cooling?
Isern, Cataln, Garca-Berro & TorresarXiv:0812.3043White dwarf luminosity function(number of WDs per brightness interval)No axionsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion BoundsToo much cold dark matter(classic scenario)TelescopeExperimentsGlobular clusters(a-g-coupling)Too manyeventsToo muchenergy lossSN 1987A (a-N-coupling)Too muchhot dark matterCAST search rangeADMXsearch rangeClassicregionAnthropicregion1031061091012 [GeV] faeVkeVmeVmeVmaneV1015 Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions
xionsAs Dark MatterGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Lee-Weinberg Curve for Neutrinos and Axions10 eV 10 meVCDMHDMAxionsThermal RelicsNon-ThermalRelics10 eVCDMHDM10 GeVNeutrinos& WIMPsThermal RelicsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Hot Dark Matter from Thermalization after LQCD
ppapChang & Choi, PLB 316 (1993) 51Hannestad, Mirizzi& Raffelt,hep-ph/0504059Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011
Power Spectrum of Cosmic Density FluctuationsTegmark, TAUP 2003Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Neutrino and Axion Hot Dark Matter Limits
Credible regions for neutrino plusaxion hot dark matter(WMAP-7, SDSS, HST)Hannestad, Mirizzi, Raffelt & Wong[arXiv:1004.0695]95%68%Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 New BBN limits on sub-MeV mass axions
Cadamuro, Hannestad, Raffelt & Redondo, arXiv:1011.3694 (JCAP) Axions essentially in thermal equilibrium throughout BBN e+e- annihilation partly heats axions missing photons Reduced photon/baryon fraction during BBN Reduced deuterium abundance, using WMAP baryon fractionGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion BoundsToo much cold dark matter(classic scenario)TelescopeExperimentsGlobular clusters(a-g-coupling)Too manyeventsToo muchenergy lossSN 1987A (a-N-coupling)Too muchhot dark matterCAST search rangeADMXsearch rangeClassicregionAnthropicregion1031061091012 [GeV] faeVkeVmeVmeVmaneV1015 Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions
xionsAs Cold Dark MatterGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Creation of Cosmological Axions
Axions are born as nonrelativistic, classical field oscillationsVery small mass, yet cold dark matterGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Cosmic Axion Field Evolution (1)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Searching for Axions in the Anthropic WindowGraham & Rajendran, arXiv:1101.2691Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Cosmic Axion Field Evolution (2)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Cosmic Axion DensityModern values for QCD parameters and temperature-dependent axion massimply (Bae, Huh & Kim, arXiv:0806.0497)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Cosmology in PLB 120 (1983)
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Killing Two Birds With One Stone
Peccei-Quinn mechanism Solves strong CP problem May provide dark matter in the form of axionsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Cold Axion PopulationsCase 2:Reheating restores PQ symmetry Case 1:Inflation after PQ symmetry breaking Isocurvature fluctuations from large quantum fluctuations of massless axion field created during inflation
Strong CMB bounds on isocurvature fluctuations
Scale of inflation required to be smallDark matter density a cosmic randomnumber (environmental parameter)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions from Cosmic Strings
Strings form by Kibble mechanism after break-down of UPQ(1) Small loops form by self-intersection Paul Shellard
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Mini Clusters
The inhomogeneities of the axion field are large, leading to bound objects,axion mini clusters. [Hogan & Rees, PLB 205 (1988) 228.] Self-coupling of axion field crucial for dynamics.Typical mini cluster properties:
Mass ~ 10-12 MsunRadius ~ 1010 cmMass fraction up to several 10%
Potentially detectable with gravitational femtolensingDistribution of axion energy density. 2-dim slice of comoving length 0.25 pc[Kolb & Tkachev, ApJ 460 (1996) L25]Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Inflation, Axions, and Anthropic SelectionGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Posterior Dark Matter Probability Distribution
Tegmark, Aguirre, Rees & Wilczek,Dimensionless constants, cosmology and other dark matters,PRD 73:023505, 2006 [astro-ph/0511774] Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions
xionsIsocurvature FluctuationsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Creation of Adiabatic vs. Isocurvature PerturbationsInflaton fieldAxion fieldSlow rollReheatingDe Sitter expansion imprintsscale invariant fluctuationsInflaton decay matter & radiationBoth fluctuate the same:Adiabatic fluctuationsInflaton decay radiationAxion field oscillates late matterMatter fluctuates relative to radiation:Entropy fluctuationsDe Sitter expansion imprintsscale invariant fluctuationsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Power Spectrum of CMB Temperature Fluctuations
Acoustic PeaksSky map of CMBR temperaturefluctuationsMultipole expansionAngular power spectrumGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Adiabatic vs. Isocurvature Temperature Fluctuations
Adapted from Fox, Pierce & Thomas, hep-th/0409059Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Parameter DegeneraciesHamann, Hannestad, Raffelt & Wong, arXiv:0904.0647
WMAP-5WMAP-5 + LSSPlanck forecastCosmic VarianceLimited (CVL)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Isocurvature Forecast
Hubble scale during inflationAxion decay constantHamann, Hannestad, Raffelt & Wong, arXiv:0904.0647Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions
xionsSolar Axion SearchesGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Experimental Tests of Invisible Axions
Pierre Sikivie:
Macroscopic B-field can provide alarge coherent transition rate overa 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, MunichISAPP, Heidelberg, 15 July 2011 Search for Solar Axions
gaSunPrimakoff productionAxion Helioscope(Sikivie 1983)gMagnet S NaAxion-Photon-OscillationTokyo 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, MunichISAPP, Heidelberg, 15 July 2011 Axion-Photon-Transitions as Particle OscillationsStationary Klein-Gordonequationfor coupleda-g-system Axions roughly like another photon polarization state In a homogeneous or slowly varying B-field, a photon beam develops a coherent axion componentRaffelt & Stodolsky, PRD 37 (1988) 1237 Photon refractive and birefringence effects (Faraday rotation, Cotton-Mouton-effect)Axion-photon transitionsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Tokyo Axion Helioscope (Sumico)
Moriyama, Minowa, Namba, Inoue, Takasu & YamamotoPLB 434 (1998) 147
Inoue, Akimoto, Ohta, Mizumoto, Yamamoto & MinowaPLB 668 (2008) 93
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 LHC Magnet Mounted as a Telescope to Follow the Sun
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 CAST at CERN
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Extending to higher mass values with gas filling
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Helioscope LimitsCAST-I results: PRL 94:121301 (2005) and JCAP 0704 (2007) 010 CAST-II results (He-4 filling): JCAP 0902 (2009) 008CAST-II results (He-3 filling): arXiv:1106.3919
First experimental crossing of the KSVZ lineGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Next Generation Axion Helioscope
I. Irastorza et al., Towards a new generation axion helioscope, arXiv:1103.5334 Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011
Helioscope ProspectsSN 1987ALimitsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axions
xionsCavity Search ExperimentsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Experimental Tests of Invisible Axions
Magnet NS
Axion field homogeneous on these scalesUse cavity to achieve large overlap integralbetween photon and axion wavesPrimakoff effect:
Axion-photon transition in externalstatic E or B field
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Search for Galactic Axions (Cold Dark Matter)
PowerFrequencymaAxion SignalThermal noise of cavity & detectorPower of galactic axion signal Microwave Energies (1 GHz 4 meV) Dark matter axions Velocities in galaxy Energies thereforema = 1-100 meVva 10-3 cEa (1 10-6) maAxion Haloscope (Sikivie 1983)Bext 8 TeslaMicrowave ResonatorQ 105Primakoff Conversion
gaBextCavityovercomesmomentummismatchGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Dark Matter Searches
1. Rochester-Brookhaven- Fermilab, PRD 40 (1989) 31532. University of Florida PRD 42 (1990) 12973. US Axion Search ApJL 571 (2002) L274. CARRACK I (Kyoto) hep-ph/01012001234Limits assuming axions are the galactic dark matter with standard halo KSVZDFSZGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 ADMX Hardware
Gianpaolo Carosi, Talk at Fermilab (May 2007)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011
SQUID Microwave Amplifiers in ADMXGianpaolo Carosi, Talk at Fermilab (May 2007)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 ADMX phase I: First-year science data (2009)
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 ADMX Moves to University of Washington
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 ADMX Schedule
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 ADMX Reach
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Dark Matter Searches
1. Rochester-Brookhaven- Fermilab, PRD 40 (1989) 31532. University of Florida PRD 42 (1990) 12973. US Axion Search ApJL 571 (2002) L274. CARRACK I (Kyoto) hep-ph/01012001234Limits assuming axions are the galactic dark matter with standard halo KSVZDFSZADMX search range (2015+)Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion BoundsToo much cold dark matter(classic scenario)TelescopeExperimentsGlobular clusters(a-g-coupling)Too manyeventsToo muchenergy lossSN 1987A (a-N-coupling)Too muchhot dark matterCAST search rangeADMXsearch rangeClassicregionAnthropicregion1031061091012 [GeV] faeVkeVmeVmeVmaneV1015 Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 R & D for Higher-Frequency Cavities
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 And if the axion be found?
Karl van Bibberat IDM 2008 Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Axion Infall
Karl van Bibberat IDM 2008 Fine Structure in the Axion Spectrum
Axion distribution on a 3-dim sheet in 6-dim phase space Is folded up by galaxy formation Velocity distribution shows narrow peaks that can be resolved More detectable information than local dark matter densityP.Sikivie& collaboratorsGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 SummaryGeorg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011 Pie Chart of Dark Universe
Dark Energy 73% (Cosmological Constant) Neutrinos 0.1-2%Dark Matter23%Ordinary Matter 4%(of this only about 10% luminous)
Georg Raffelt, MPI Physics, MunichISAPP, Heidelberg, 15 July 2011