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Axions in the Skies

Axions in the Skies. Supernova 1987A. Globular Cluster. TeV Gamma Rays. Gravity Waves. Solar Axions. Georg G. Raffelt, Max-Planck-Institut f ür Physik, München. High- and Low-Energy Frontiers in Particle Physics. QCD scale. Planck mass. Cosmological constant. Electroweak scale. GUT

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Axions in the Skies

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  1. Axions in the Skies Supernova 1987A Globular Cluster TeV Gamma Rays Gravity Waves Solar Axions Georg G. Raffelt, Max-Planck-Institut für Physik, München

  2. High- and Low-Energy Frontiers in Particle Physics QCD scale Planck mass Cosmological constant Electroweak scale GUT scale Cosmic rays eV CERN 22 mg “Intensity Frontier” (feeble interactions) Low-E Frontier High-Energy Frontier

  3. High- and Low-Energy Frontiers in Particle Physics QCD scale Planck mass Cosmological constant Electroweak scale GUT scale eV Heavy right-handed neutrinos (see-saw mechanism) Axion dark matter(related to Peccei-Quinn symmetry)

  4. High- and Low-Energy Frontiers in Particle Physics QCD scale Planck mass Cosmological constant Electroweak scale GUT scale eV Black Hole Super-Radiance AxDM Allowed fa SR Experimental & Astro Limits Axion dark matter(related to Peccei-Quinn symmetry)

  5. Super-Radiance Masha Baryakhtar, Talk at Invisibles 2016, https://indico.cern.ch/event/464402/

  6. Super-Radiance Masha Baryakhtar, Talk at Invisibles 2016, https://indico.cern.ch/event/464402/

  7. Gravitational Wave Signals • Arvanitaki,Baryakhtar, Dimopoulos,Dubovsky &Lasenby, arXiv:1604.03958 Masha Baryakhtar, Talk at Invisibles 2016, https://indico.cern.ch/event/464402/

  8. High- and Low-Energy Frontiers in Particle Physics QCD scale Planck mass Cosmological constant Electroweak scale GUT scale eV Grav.Waves from BHs AxDM Allowed fa SR Experimental & Astro Limits Axion dark matter(related to Peccei-Quinn symmetry)

  9. Solar Models Solar Axions and Axion-Like Particles

  10. Phenomenological Axion Properties Gluon coupling (generic), defines normalization of axion scale Mass (generic) depends on up/down quark masses Axion-photon coupling (model dependent) Generic from -- mixing Model-dependent, E/N = 0 (KSVZ), 8/3 (DFSZ), many others Axion-nucleon coupling (model-dependent numerical factors ) Axion-electron coupling in non-hadronic models is analogous with • Axial-vector current • Spin-dependent int’n

  11. First discussion of Primakoff effect for WW axions () For “invisible axions” () screening effects crucial (G.R., PRD 33, 897:1986)

  12. Solar Observables Modified by Axion Losses New opacity Old opacity Surface He abundance Depth Convective Zone Boron neutrinos Beryllium neutrinos Vinyoles, Serenelli, Villante, Basu, Redondo & Isern, arXiv:1501.01639

  13. Solar Sound-Speed Variation New opacity New energy loss makes disagreement with seismic observations worse, especially in the central regions Vinyoles, Serenelli, Villante, Basu, Redondo & Isern, arXiv:1501.01639

  14. Global Fit from Solar Observables Allow all input parameters to float, including chemical composition, and marginalize except for axion losses Vinyoles, Serenelli, Villante, Basu, Redondo & Isern, arXiv:1501.01639

  15. Experimental Tests of Invisible Axions Primakoff effect: Axion-photon transition in external static E or B field (Originally discussed for by Henri Primakoff 1951) • 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

  16. Search for Solar Axions Axion Helioscope (Sikivie 1983) Primakoff production N Axion flux a a g g MagnetS Axion-Photon-Oscillation Sun • Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008) • 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 ...)

  17. LHC Magnet Mounted as a Telescope to Follow the Sun

  18. CAST Results

  19. Parameter Space for Axion-Like Particles (ALPs) Two parameters: - ALP mass - ALP- coupling Weinberg Wilczek “standard axion” Model dependence (KSVZ, DFSZ, …) broadens the “axion line”

  20. Parameter Space for Axion-Like Particles (ALPs) CAST exclusion range End of solar spectrum Large , --oscillations suppressed --oscillations enhanced with He filling () Maximal mixing (“coherent”, small )

  21. Next Generation Axion Helioscope (IAXO) Need new magnet w/ – Much bigger aperture: per bore – Lighter (no iron yoke) – Bores at Troom • Irastorza et al.: Towards a new generation axion helioscope, arXiv:1103.5334 • Armengaud et al.: Conceptual Design of the International Axion Observatory (IAXO), arXiv:1401.3233

  22. Parameter Space for Axion-Like Particles (ALPs) - Improvement by a factor of 30 - Leaping into uncharted territory QCD Axion meV frontier Pushing generic ALP frontier

  23. Axion Dark Matter from Topological Defects Editor’s suggestion Diversity of scenarios for cosmic axion production depending on domain-wall index NDW and phase parameter δ of the bias term

  24. Historical Neutrino Dark Matter Lessons Early 1980s - If neutrinos have mass, probably they are dark matter () (“Neutrinos are known to exist”, only SM candidate) - Detection of at ITEP, Moscow (PRL 58:2019, 1987) - Dedicated oscillation experiments (NOMAD 1995–1998 and CHORUS 1994–1997) Status 2015 - 70% of gravitating “mass” is dark energy - Dark matter must be mostly “cold” (structure formation) - Neutrinos have sub-eV masses (oscillations, cosmo limits) - Sub-dominant dark matter component History does not always repeat itself, but … - If axions (or similar) exist, MUST be ALL of dark matter?

  25. Gamma-ALP Conversion in Astrophysical B-Fields Credit: SLAC National Accelerator Laboratory/Chris Smith http://svs.gsfc.nasa.gov/vis/a010000/a012300/a012317/

  26. Axion-Photon-Conversion from SN 1987A Axion-photon conversion in transverse galactic B-field SN 1987A SMM No excess g rays in coincidence with SN 1987A Primakoff production in SN core Galactic B-field models Payez, Evoli, Fischer, Giannotti, Mirizzi & Ringwald, arXiv:1410.3747

  27. Astrophysical ALP-Photon Conversion Galactic and cluster fields (mG range) or intergalactic (nG) can cause significant conversion over kpc–Mpc scales: Low-mass ALPs Manuel Meyer, arXiv:1611.07784

  28. Hillas Plot A. M. Hillas Ann. Rev. Astron. Astrophys. 22, 425 (1984) Size and B field strength of possible sites for particle acceleration. Objects below the line cannot accelerate protons to 1020 eV ALP-gconversion

  29. Galactic Globular Cluster M55

  30. Color-Magnitude Diagram for Globular Clusters H H He C O He Asymptotic Giant Red Giant H H He C O White Dwarfs Horizontal Branch Main-Sequence Particle emission reduces helium burning lifetime, i.e. number of HB stars Hot, blue cold, red Color-magnitude diagram synthesized from several low-metallicity globular clusters and compared with theoretical isochrones (W.Harris, 2000)

  31. New ALP Limits from Globular Clusters Helium abundance and energy loss rate from modern number counts HB/RGB in 39 globular clusters Planck Ayala, Dominguez, Giannotti, Mirizzi & Straniero, arXiv:1406.6053

  32. Parameter Space for Axion-Like Particles (ALPs)

  33. Axion-Electron Interaction • Axions can interact with electrons, notably in GUT models, e.g. DFSZ model • Strong constraints from stars Electrons Compton Pair Annihilation Electromagnetic Bremsstrahlung

  34. Color-Magnitude Diagram of Globular Cluster M5 Brightest red giant measures nonstandard energy loss CMD (a) before and (b) after cleaning CMD of brightest 2.5 mag of RGB Viaux, Catelan, Stetson, Raffelt, Redondo, Valcarce & Weiss, arXiv:1308.4627

  35. Limits on Axion-Electron Coupling from GC M5 I-band brightness of tip of red-giant brach [magnitudes] Detailed account of theoretical and observational uncertainties • Uncertainty dominated by distance • Can be improved in future (GAIA mission) Axion-electron Yukawa Limit on axion-electron Yukawa Mass limit in DFSZ model Viaux, Catelan, Stetson, Raffelt, Redondo, Valcarce & Weiss, arXiv:1311.1669

  36. Axion Bounds from WD Luminosity Function Limits on axion-electron coupling and mass limit in DFSZ model: Miller Bertolami, Melendez, Althaus & Isern, arXiv:1406.7712, 1410.1677

  37. Period Change of Variable White Dwarfs Period change of pulsating white darfs depends on cooling speed White dwarf G117−B15A White dwarf PG 1351+489 Favored by Limited by Córsico et al., arXiv:1205.6180 Battich et al., arXiv:1605.07668

  38. Summary of White Dwarf Bounds Tip of RGB Luminosity Function Period Change Variable White Dwarfs Córsico et al., arXiv:1605.06458

  39. Neutrinos from Thermal Processes Photo (Compton) Plasmon decay Pair annihilation Bremsstrahlung These processes were first discussed in 1961-63 after V-A theory

  40. Neutrino-Photon-Coupling in a Plasma Neutrino effective in-medium coupling For vector current it is analogous to photon polarization tensor Emission almost purely electron flavor for for and

  41. Sanduleak -69 202 Sanduleak -69 202 Supernova 1987A 23 February 1987

  42. Supernova 1987A Energy-Loss Argument SN 1987A neutrino signal Neutrino sphere Volume emission of new particles Neutrino diffusion Emission of very weakly interacting particles would “steal” energy from the neutrino burst and shorten it. (Early neutrino burst powered by accretion, not sensitive to volume energy loss.) Late-time signal most sensitive observable

  43. Three Phases of Neutrino Emission Explosion triggered Cooling on neutrino diffusion time scale • Shock breakout • De-leptonization of • outer core layers • Shock stalls 150 km • Neutrinos powered by • infalling matter Spherically symmetric Garching model (25M⊙) with Boltzmann neutrino transport

  44. Cooling Time Scale Exponential cooling model: T = T0 e-t/4, constant radius, L = L0 e-t/ Fit parameters are T0, , radius, 3 offset times for KII, IMB & BST detectors Loredo and Lamb, Bayesian analysis astro-ph/0107260

  45. Long-Term Cooling of EC SN (Garching 2009) Neutrino opacities with strong NN correlations and nucleon recoil in neutrino-nucleon scattering. Exponential cooling with Barely allowed by SN 1987A Neutrino opacities without these effects Much longer cooling times L. Hüdepohl et al. (Garching Group),arXiv:0912.0260

  46. Axion Emission from a Nuclear Medium Axion-nucleon interaction: a Energy-loss rate( (axion energy ) Dynamical structure function, in nonrelativistic limit correlator of nucleon spin density operator N N + ... V N N Nucleon-Nucleon Bremsstrahlung Early calculations using one-pion exchange potential without many body effects or multiple-scattering effects over-estimated emission rate, see e.g. • Janka, Keil, Raffelt & Seckel, PRL 76:2621,1996. • Hanhart, Phillips & Reddy, PLB 499:9, 2001. • Bacca, Hally, Liebendörfer, Perego, Pethick & Schwenk, ApJ 758: 34 (2012). • Bartl, Pethick & Schwenk, PRL 113:081101 (2014).

  47. Axion-Nucleon Couplings Axion-nucleon coupling (model-dependent numerical factors ) Axion-electron coupling in non-hadronic models is analogous with • Axial-vector current • Spin-dependent int’n Values from Grilli di Cortona et al. arXiv:1511.02867 Coupling to neutron could be very small!

  48. Axion Bounds and Searches [GeV] fa 103 106 109 1012 1015 keV eV meV meV neV ma Microwave Searches CASPEr Experiments Tele scope CAST Hadronic axions String DW Too much CDM (misalignment) Too much cold dark matter (re-alignment with Qi = 1) Too much hot darkmatter Helium-burning stars (a-g-coupling, hadronic axions) SN 1987A Too many events Too much energy loss Globular clusters (He ignition), WD cooling (a-e coupling)

  49. Diffuse Supernova Axion Background (DSAB) • 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 measured • Axions with • near SN 1987A energy-loss limit • Provide DSAB with compable • energy density as DSNB and EBL • No obvious detection channel Raffelt, Redondo & Viaux work in progress (2011)

  50. Cooling of Neutron Star in Cas A Chandra x-ray image of non-pulsar compact remnant Measured surface temperature over 10 years reveals unusually fast cooling rate • Neutron Cooper pair breaking and formation (PBF) as neutrino emission process? • Evidence for extra cooling (by axions)? Leinson, arXiv:1405.6873

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