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The Search for Axions

This conference and colloquium, held on December 5, 2016, delved into the motivation, properties, production, and detection of axions as a form of dark matter. The event also discussed the Strong CP Problem, exploring the absence of P and CP violation in strong interactions and the intriguing implications it poses. Various topics discussed include axion constraints, laboratory searches, cosmological implications, and axion search techniques like the cavity haloscope and axion helioscope. The conference highlighted the latest advancements in axion research and detection technology, emphasizing the significance of axions in the study of dark matter and fundamental physics.

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The Search for Axions

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  1. The Search for Axions Pierre Sikivie Axion Dark Matter Conference & Oscar Klein Centre Colloquium December 5, 2016

  2. Outline • Axion motivation and properties • Production in the early universe • Axion dark matter detection • Other methods

  3. The Strong CP Problem where The absence of P and CP violation in the strong interactions requires from upper limit on the neutron electric dipole moment

  4. A level pooltable on an inclined floor g

  5. The Standard Model does not provide a reason for to be so tiny, but a relatively small modification does …

  6. is a symmetry of the classical action is spontaneously broken has a color anomaly Peccei and Quinn, 1977

  7. If a symmetry is assumed, relaxes to zero, and a light neutral pseudoscalar particle is predicted: the axion. Weinberg, Wilczek 1978

  8. A self adjusting pooltable g 1 ton

  9. f f a a = 0.97 in KSVZ model 0.36 in DFSZ model

  10. Searching for the pooltable oscillation quantum g 1 ton

  11. Axions are constrained by • beam dump experiments • rare particle decays • radiative corrections • the evolution of stars

  12. from G. Raffelt, 0611350

  13. The remaining axion window laboratory searches cosmology stellar evolution

  14. g a Thermal axions q these processes imply an axion decoupling temperature thermal axion temperature today: = effective number of thermal degrees of freedom at axion decoupling

  15. There are two cosmic axion populations: hot and cold. When the axion mass turns on, at QCD time,

  16. V Effective potential V(T, ) axion strings axion domain walls

  17. Axion production by vacuum realignment V V a a initial misalignment angle J. Preskill, M. Wise & F. Wilczek, L. Abbott & PS, M. Dine & W. Fischler, 1983

  18. A self adjusting pooltable g 1 ton

  19. . If inflation after the PQ phase transition . produces isocurvature density perturbations may be accidentally suppressed CMBR constraint

  20. . If no inflation after the PQ phase transition . S. Borsanyi et al. 1606.07494 axion miniclusters appear cold axions are produced by vacuum realignment, string decay and wall decay

  21. Axions are cold dark matter Density Velocity dispersion Effective temperature

  22. Searching for relic pooltable oscillations g 1 ton

  23. Axion Search Techniques the cavity haloscope the axion helioscope shining light through walls axion mediated long-range forces NMR methods LC circuit atomic transitions

  24. Axion dark matter is detectable PS '83 a X FFT A/D

  25. conversion power on resonance search rate for s/n = 4

  26. Axion Dark Matter eXperiment

  27. ADMX hardware high Q cavity experimental insert

  28. *Supported by DOE Grants DE-FG02-97ER41029, DE-FG02-96ER40956, DE-AC52-07NA27344, DE-AC03-76SF00098, NSF Grant PHY-1067242, and the Livermore LDRD program ADMX in its second generation

  29. Upgrade with SQUID Amplifiers IB The basic SQUID amplifier is a flux-to-voltage transducer SQUID noise arises from Nyquist noise in shunt resistance scales linearly with T However, SQUIDs of conventional design are poor amplifiers above 100 MHz (parasitic couplings). Vo (t) F Flux-bias to here

  30. Quantum-limited SQUID-based amplification • SQUIDs have been measured with TN ~ 50 mK • Compared to ~ 2 K for HFET amplifiers • Near quantum– limited noise • Provides a large increase in ADMX sensitivity SQUID amplifiers J. Clarke et al.

  31. Gen 2 ADMX sensitivity Will scan the lower-mass decade at or below DFSZ sensitivity

  32. ADMX-HF at Yale • Multi-post system that consists of 3 rotors connected on common axis and 3 stators. • 4” ID cavity: Six 0.5” diameter rods • Freq. span 4.7- 6.0 GHz

  33. B. Brubaker et al., arXiv: 1610.02580

  34. Center for Axion and Precision Physics (CAPP) in Korea

  35. Axion Search Techniques the cavity haloscope the axion helioscope shining light through walls axion mediated long-range forces NMR methods LC circuit atomic transitions

  36. a Axion to photon conversion in a magnetic field x Theory P. S. ’83 L. Maiani, R. Petronzio and E. Zavattini ’86 K. van Bibber et al. ’87 G. Raffelt and L. Stodolsky, ‘88 K. van Bibber et al. ’89 Experiment D. Lazarus et al. ’92 R. Cameron et al. ‘93 S. Moriyama et al. ’98, Y. Inoue et al. ’02 K. Zioutas et al. 04 E. Zavattini et al. 05 conversion probability with

  37. Tokyo Axion Helioscope

  38. CernAxionSolarTelescope Sunset Photon detectors Sunrise Photon detectors Sunrise axions Sunset axions Decommissioned LCH test magnet Rotating platform 3 X-ray detectors X-ray Focusing Device

  39. CAST Collaboration: Phys. Rev. Lett. 112 (2013) 091302

  40. Solax, Cosme ’98 Primakoff conversion of solar axions in crystals on Earth a Ge DAMA ‘01 x NaI (100 kg) CDMS ‘09 fewkeV Ge Bragg scattering on crystal lattice Edelweiss ‘13 Ge

  41. from C. Eleftheriadis (CAST), arXiv: 0706.0637

  42. Axio-Electric Effect • Theory • Experiment S. Dimopoulos, G.D. Starkman & B.W. Lynn, '86 F. Avignone et al., '87 E. Aprile et al., '09 E. Armengaud et al. ‘13

  43. Linearly polarized light in a constant magnetic field

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