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