Axion

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Axion
InteractionsGravity, Electromagnetic
StatusHypothetical
Theorized1977, Peccei and Quinn
Mass10−6 to 1 eV/c2
Electric charge0
Spin0
 
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Axion
InteractionsGravity, Electromagnetic
StatusHypothetical
Theorized1977, Peccei and Quinn
Mass10−6 to 1 eV/c2
Electric charge0
Spin0

The axion is a hypothetical elementary particle postulated by the Peccei–Quinn theory in 1977 to resolve the strong CP problem in quantum chromodynamics (QCD). If axions exist and have low mass within a specific range, they are of interest as a possible component of cold dark matter.

Contents

History

Reasons for prediction

As shown by Gerardus 't Hooft, strong interactions of the standard model, QCD, possess a non-trivial vacuum structure that in principle permits the violation of the combined symmetries of charge conjugation and parity, collectively known as CP. Together with effects generated by the weak interactions, the effective strong CP violating term, Θ, appears as a Standard Model input parameter—it is not predicted by the theory, but must be measured. However, large CP violating interactions originating from QCD would induce a large electric dipole moment for the neutron. (While the neutron is an electrically neutral particle, nothing prevents charge separation within the neutron itself.) Experimental constraints on the currently unobserved neutron's electric dipole moment imply that CP violation arising from QCD must be extremely tiny and thus Θ must itself be extremely small or absent. Since a priori Θ could have any value between 0 and 2π (the parameter is periodic), this presents a naturalness problem for the standard model. Why should this parameter find itself so close to 0? (Or, why should QCD find itself CP-preserving?) This question constitutes what is known as the strong CP problem.

One simple solution exists: if at least one of the quarks of the standard model is massless, Θ becomes unobservable; i.e. it vanishes from the theory. However, empirical evidence strongly suggests that none of the quarks is massless and so the strong CP problem persists.

In 1977, Roberto Peccei and Helen Quinn postulated a more elegant solution to the strong CP problem, the Peccei–Quinn mechanism. The idea is to effectively promote Θ to a field (particle). This is accomplished by adding a new global symmetry (called a Peccei–Quinn symmetry) to the standard model that becomes spontaneously broken. Once this new global symmetry breaks, a new particle results and, as shown by Frank Wilczek and Steven Weinberg, this particle fills the role of Θ—naturally relaxing the CP violation parameter to zero. This hypothesized new particle is called the axion. (On a more technical note, the axion is the would-be Nambu–Goldstone boson that results from the spontaneously broken Peccei–Quinn symmetry. However, the non-trivial QCD vacuum effects (instantons) spoil the Peccei–Quinn symmetry explicitly and provide a small mass for the axion. Hence, the axion is actually a pseudo-Nambu–Goldstone boson.)

Experimental searches

A number of experiments have attempted to detect axions, including at least one that has claimed positive results.

In the Italian PVLAS experiment polarized light propagates through the magnetic field of a 5T dipole magnet, searching for a small anomalous rotation of the direction of polarization. The concept of the experiment was first put forward in 1986 by Luciano Maiani, Roberto Petronzio and Emilio Zavattini,[1] and if axions exist, photons could interact with the field to become virtual or real axions. This rotation is very small and difficult to detect, but this problem can be overcome by reflecting light back and forth through the magnetic field millions of times. The most recent PVLAS results do detect an anomalous rotation, which can be interpreted in terms of an axion of mass 1–1.5 meV. However, there are other possible sources for such an effect besides axions.[2]

Several experiments search for axions of astrophysical origin using the Primakoff effect. This effect causes conversions of axions to photons and vice versa in strong electromagnetic fields. Axions can be produced in the Sun's core when X-rays scatter off electrons and protons in the presence of strong electric fields and are converted to axions. The CAST experiment is currently underway to detect these axions by converting them back to x rays in a strong magnetic field.

The Axion Dark Matter Experiment (ADMX) searches for light, weakly interacting axions saturating the dark matter halo of our galaxy.[3] ADMX is a strong magnetic field permeating a cold microwave cavity. Axions matching the resonant frequency of the cavity decay into microwave photons. ADMX has excluded optimistic axion models in the 1.9 μeV to 3.53 μeV range.[4]

Another means of searching for axions is by conducting so called "light shining through walls" experiments,[5] where a beam of light is passed through an intense magnetic field in an attempt to observe the conversion of photons into axions by allowing them to pass through an aluminium plate, blocking the passage of photons. However, these practices are of low efficacy, necessitate high initial photon flux, and those conducted by BFRS and PVLAS have been the subject of some further verification.[6] A recent experiment had the necessary sensitivity to detect this effect if the PVLAS 2005-signal was due to axions; however, no effect was seen.[6]

On 9 July 2007, a paper submitted to arXiv by Carlo Rizzo[6] and other researchers from the Centre National de la Recherche Scientifique indicated with a confidence level of 94% or higher, that they believed the results published by the PVLAS experiment, in Italy, were incorrect and did not prove the existence of the axion.[6] Initially, the team researched the matter after their claim that the axion coupling inferred from the PVLAS experiment did not match with experiments conducted in 2007 and earlier in 2006,[7] and thus required review.[6]

The experiment conducted by Rizzo's team differed from the approach of the Italian researchers in the fact that at the end of a vacuum chamber, an aluminium plate was placed[6] to prevent photons from an adjacent laser from passing through the plate, where axions would simply pass through the plate and be converted back into photons,[6] and were able to observe a small-portion of the supposed-converting particles—to the number of 4×1022 photons.[6]

In the use of optical measurement and pulsating beams of light, the team showed through illustration of exclusion curves compared to the PVLAS experiment and another conducted by the BFRT,[6] that the axion had been ruled out but still remained a valid hypothesis;[6] the experiment counting as an important step in the understanding of the particle, with the possibility of a very weak coupled axion.[6]

A few days earlier, on the 23 June, the PVLAS had submitted a paper to arXiv,[8] in which they noted that upgrades to their measurement systems had been undertaken to increase the accuracy of their results from the previous year,[8] through the use of 2.3 and 5.5 T fields[8] and wavelengths of 1064 nm.[8] With this increased accuracy, PVLAS had noted that the axion particle interpretation had been ruled out[8] due to the absence of a rotational signal on the levels of 1.2×10−8 rad×5.5 T and 1.0×10−8 rad×2.3 T with 45,000 passes.[8]

Axions and other light bosons are also expected to have an observable signature in various astrophysical settings. In particular, several recent works have proposed the existence of axion-like particles as a possible solution to the apparent transparency of the Universe to TeV gamma-ray radiation.[9][10] It has also been demonstrated in a few recent works that, on accounts of the large magnetic fields threading the atmospheres of compact astrophysical objects (e.g., magnetars), such environments will convert photons to axions much more efficiently than most laboratory experiments, over a broad axion mass range. This, in turn, would give rise to distinct absorption-like features in the spectra of such objects which can be observed by current telescopes and, therefore, significantly increase our sensitivity to axion detection.[11] A new promising detection means for axions and axion-like particles is by looking for quasi-particle beam refraction effects in systems with strong magnetic field gradients such as radio-loud magnetars and magnetic pulsars. In particular, the refraction effects will lead to beam splitting effects that can be easily detected in the radio light curves of highly magnetized pulsars and could allow for the detection of light bosons with much greater sensitivities than are currently achievable by other means.[12]

A pair of papers by Katherine Mack that appeared on the arXiv in November 2009 casts doubt on the existence of the QCD axion lighter than μeV scale, arguing that (1) cosmological observations imply that the existence of such a light axion creates a greater fine-tuning problem than the one that it was hypothesized to solve[13] and (2) that anthropic arguments do not alleviate this fine-tuning problem.[14] These papers argue that, since the very motivation for the axion was to fix a fine-tuning problem, but the existence of very light axion(s) creates a different, and larger, fine-tuning problem—and, moreover, since the axion has never been observed—there is no longer any good reason to suspect that axions of mass below μeV scale exist.

Axions in condensed-matter physics

A term analogous to the one that must be added to Maxwell's equations[15] also appears in recent theoretical models for topological insulators.[16] This term leads to several interesting predicted properties at the interface between topological and normal insulators.[17] In this situation the field θ describes something very different from its use in high-energy physics.[17]

Properties

Predictions

One theory of axions relevant to cosmology had predicted that they would have no electric charge, a very small mass in the range from 10−6 to 1 eV/c2, and very low interaction cross-sections for strong and weak forces. Because of their properties, axions interact only minimally with ordinary matter. Axions are predicted to change to and from photons in the presence of strong magnetic fields, and this property is used for creating experiments to detect axions.

Supersymmetry

In supersymmetric theories the axion has both a scalar and a fermionic superpartner. The fermionic superpartner of the axion is called the axino, the scalar superpartner is called the saxion. In some models, the saxion is the dilaton. They are all bundled up in a chiral superfield.

The axino has been predicted to be the lightest supersymmetric particle in such a model.[18] In part due to this property, it is considered a candidate for the composition of dark matter.[19]

Cosmological implications

Theory suggests that axions were created abundantly during the Big Bang. Because of a unique coupling to the instanton field of the primordial universe (the "misalignment mechanism"), an effective dynamical friction is created during the acquisition of mass following cosmic inflation. This robs all such primordial axions of their kinetic energy.

If axions have low mass, thus preventing other decay modes, axion theories predict that the universe would be filled with a very cold Bose-Einstein condensate of primordial axions. Hence, depending on their mass, axions could plausibly explain the dark matter problem of physical cosmology.[20] Observational studies to detect dark matter axions are underway, but they are not yet sufficiently sensitive to probe the mass regions where axions would be expected to be found if they are the solution to the dark matter problem. The microwave cavity experiment known as ADMX in 1996–2010 failed to detect axions having a mass range of 1.98–2.17 µeV and a frequency between 450 and 850 MHz.[21] High mass axions of the kind searched for by Jain and Singh (2007)[22] would not persist in the modern universe and could not contribute to dark matter.

Low mass axions could have additional structure at the galactic scale. As they continuously fell into a galaxy from the intergalactic medium, they might be denser in "caustic" rings.[23] The gravitational effects of these rings on galactic structure and rotation might then be observable.[24] Other cold dark matter theoretical candidates, such as WIMPs and MACHOs, would also form such rings, but, because such candidates are fermionic, the rings would be less pronounced than with bosons such as the axion.

References

Notes

  1. ^ Maiani, L.; Petronzio; Zavattini, E. (1986). "Effects of nearly massless, spin-zero particles on light propagation in a magnetic field". Phys. Lett. 175 (3): 359–363. Bibcode 1986PhLB..175..359M. doi:10.1016/0370-2693(86)90869-5.
  2. ^ Steve Reucroft, John Swain. Axion signature may be QED CERN Courier, 2006-10-05
  3. ^ Duffy, L. D.; Sikivie, P.; Tanner, D. B.; Bradley, R. F. (2006). "High resolution search for dark-matter axions". Physical Review D 74. arXiv:astro-ph/0603108. Bibcode 2006PhRvD..74a2006D. doi:10.1103/PhysRevD.74.012006.
  4. ^ Asztalos, S. J.; Carosi, G.; Hagmann, C.; Kinion, D.; Van Bibber, K.; Hoskins, J.; Hwang, J.; Sikivie, P. et al. (2010). "SQUID-Based Microwave Cavity Search for Dark-Matter Axions". Physical Review Letters 104 (4). arXiv:0910.5914. Bibcode 2010PhRvL.104d1301A. doi:10.1103/PhysRevLett.104.041301.
  5. ^ Ringwald, A. (2003). "Fundamental Physics at an X-Ray Free Electron Laser". Workshop on Electromagnetic Probes of Fundamental Physics (Erice, Italy): 63–74. arXiv:hep-ph/0112254. doi:10.1142/9789812704214_0007.
  6. ^ a b c d e f g h i j k Robilliard, C.; Battesti, R.; Fouche, M.; Mauchain, J.; Sautivet, A.-M.; Amiranoff, F.; Rizzo, C. (2007). "No "Light Shining through a Wall": Results from a Photoregeneration Experiment". Physical Review Letters 99 (19). arXiv:0707.1296. Bibcode 2007PhRvL..99s0403R. doi:10.1103/PhysRevLett.99.190403.
  7. ^ Andriamonje,S., et al. (CAST Collaboration), Journal of Cosmological Astroparticle Physics 4, 10 (2007); Duffy, L. D, et al., Physical Review D, vol 74, 110406 (2006)
  8. ^ a b c d e f Zavattini, E.; Zavattini, G.; Ruoso, G.; Polacco, E.; Milotti, E.; Karuza, M.; Gastaldi, U.; Di Domenico, G. et al. (2006). "Experimental Observation of Optical Rotation Generated in Vacuum by a Magnetic Field". Physical Review Letters 96 (11). arXiv:hep-ex/0507107. Bibcode 2006PhRvL..96k0406Z. doi:10.1103/PhysRevLett.96.110406.
  9. ^ De Angelis, A.; Mansutti, O.; Roncadelli, M. (2007). "Evidence for a new light spin-zero boson from cosmological gamma-ray propagation?". Physical Review D 76: 121301. arXiv:0707.4312. Bibcode 2007PhRvD..76l1301D. doi:10.1103/PhysRevD.76.121301.
  10. ^ De Angelis, A.; Mansutti, O.; Persic, M.; Roncadelli, M. (2009). "Photon propagation and the very high energy gamma-ray spectra of blazars: How transparent is the Universe?". Monthly Notices of the Royal Astronomical Society: Letters 394: L21–L25. arXiv:0807.4246. Bibcode 2009MNRAS.394L..21D. doi:10.1111/j.1745-3933.2008.00602.x.
  11. ^ Chelouche, Doron; Rabadan, Raul; Pavlov, Sergey S.; Castejon, Francisco (2009). "Spectral Signatures of Photon-Particle Oscillations from Celestial Objects". The Astrophysical Journal Supplement Series 180: 1–29. arXiv:0806.0411. Bibcode 2009ApJS..180....1C. doi:10.1088/0067-0049/180/1/1.
  12. ^ Chelouche, Doron; Guendelman, Eduardo I. (2009). "COSMIC ANALOGS OF THE STERN-GERLACH EXPERIMENT AND THE DETECTION OF LIGHT BOSONS". The Astrophysical Journal 699: L5–L8. arXiv:0810.3002. Bibcode 2009ApJ...699L...5C. doi:10.1088/0004-637X/699/1/L5.
  13. ^ Katherine J. Mack & Paul J. Steinhardt, Cosmological Problems with Multiple Axion-like Fields,preprint
  14. ^ Katherine J. Mack, Axions, Inflation and the Anthropic Principle,preprint
  15. ^ Wilczek, Frank (1987-05-04). "Two applications of axion electrodynamics". Physical Review Letters 58 (18): 1799–1802. Bibcode 1987PhRvL..58.1799W. doi:10.1103/PhysRevLett.58.1799. PMID 10034541.
  16. ^ Qi, Xiao-Liang; Taylor L. Hughes, Shou-Cheng Zhang (2008-11-24). "Topological field theory of time-reversal invariant insulators". Physical Review B 78 (19): 195424. arXiv:0802.3537. Bibcode 2008PhRvB..78s5424Q. doi:10.1103/PhysRevB.78.195424.
  17. ^ a b Franz, Marcel (2008-11-24). "High-energy physics in a new guise". Physics 1: 36. Bibcode 2008PhyOJ...1...36F. doi:10.1103/Physics.1.36.
  18. ^ Abe, Nobutaka, Takeo Moroi and Masahiro Yamaguchi (2002). "Anomaly-Mediated Supersymmetry Breaking with Axion". Journal of High Energy Physics 1: 10. arXiv:hep-ph/0111155. Bibcode 2002JHEP...01..010A. doi:10.1088/1126-6708/2002/01/010.
  19. ^ Hooper, Dan and Lian-Tao Wang (2004). "Possible evidence for axino dark matter in the galactic bulge". Physical Review D 70 (6): 063506. arXiv:hep-ph/0402220. Bibcode 2004PhRvD..70f3506H. doi:10.1103/PhysRevD.70.063506.
  20. ^ P. Sikivie,Dark matter axions,arXiv.
  21. ^ Phase 1 Results, dated 2006-03-04
  22. ^ P. L. Jain, G. Singh, Search for new particles decaying into electron pairs of mass below 100 MeV/c2, J. Phys. G: Nucl. Part. Phys., 34, 129–138, (2007); doi:10.1088/0954-3899/34/1/009, (possible early evidence of 7±1 and 19±1 MeV axions of less than 10−13 s lifetime).
  23. ^ P. Sikivie, "Dark matter axions and caustic rings"
  24. ^ P. Sikivie (personal website): pictures of alleged triangular structure in Milky Way; hypothetical flow diagram which could give rise to such a structure.

Journal entries

External links