# Chameleon particle

The chameleon is a hypothetical scalar particle that couples to matter more weakly than gravity,[1] postulated as a dark energy candidate.[2] Due to a non-linear self-interaction, it has a variable effective mass which is an increasing function of the ambient energy density—as a result, the range of the force mediated by the particle is predicted to be very small in regions of high density (for example on Earth, where it is less than 1mm) but much larger in low-density intergalactic regions: out in the cosmos chameleon models permit a range of up to several thousand parsecs. As a result of this variable mass, the hypothetical fifth force mediated by the chameleon is able to evade current constraints on equivalence principle violation derived from terrestrial experiments even if it couples to matter with a strength equal or greater than that of gravity. Although this property would allow the chameleon to drive the currently observed acceleration of the universe's expansion, it also makes it very difficult to test for experimentally.

Composition Unknown Gravity, electroweak Hypothetical Variable, depending on ambient energy density 0 0

## Hypothetical properties

Chameleon particles were proposed in 2003 by Khoury and Weltman.

In most theories, chameleons have a mass that scales as some power of the local energy density: ${\displaystyle m_{\text{eff}}\sim \rho ^{\alpha }}$ , where ${\displaystyle \alpha \simeq 1}$ .

Chameleons also couple to photons, allowing photons and chameleons to oscillate between each other in the presence of an external magnetic field.[3]

Chameleons can be confined in hollow containers because their mass increases rapidly as they penetrate the container wall, causing them to reflect. One strategy to search experimentally for chameleons is to direct photons into a cavity, confining the chameleons produced, and then to switch off the light source. Chameleons would be indicated by the presence of an afterglow as they decay back into photons.[4]

## Experimental searches

A number of experiments have attempted to detect chameleons along with axions.[5]

The GammeV experiment[6] is a search for axions, but has been used to look for chameleons too. It consists of a cylindrical chamber inserted in a 5 T magnetic field. The ends of the chamber are glass windows, allowing light from a laser to enter and afterglow to exit. GammeV set the limited coupling to photons in 2009.[7]

CHASE (CHameleon Afterglow SEarch) results published in November 2010,[8] improve the limits on mass by 2 orders of magnitude and 5 orders for photon coupling.

A 2014 neutron mirror measurement excluded chameleon field for values of the coupling constant ${\displaystyle \beta >5.8\times 10^{8}}$ ,[9] where the effective potential of the chameleon quanta is written as ${\displaystyle V_{\text{eff}}=V(\Phi )+e^{\beta \Phi /M'_{\text{P}}}\rho }$ , ${\displaystyle \rho }$  being the mass density of the environment, ${\displaystyle V(\Phi )}$  the chameleon potential and ${\displaystyle M'_{\text{P}}}$  the reduced Planck mass.

The CERN Axion Solar Telescope has been suggested as a tool for detecting chameleons.[10]

## References

### Notes

1. ^ Cho, Adrian (2015). "Tiny fountain of atoms sparks big insights into dark energy". Science. doi:10.1126/science.aad1653.
2. ^ Khoury, Justin; Weltman, Amanda (2004). "Chameleon cosmology". Physical Review D. 69 (4): 044026. arXiv:astro-ph/0309411. Bibcode:2004PhRvD..69d4026K. doi:10.1103/PhysRevD.69.044026.
3. ^ Erickcek, A. L.; Barnaby, N; Burrage, C; Huang, Z (2013). "Catastrophic consequences of kicking the chameleon". Physical Review Letters. 110 (17): 171101. arXiv:1204.1488. Bibcode:2013PhRvL.110b1101S. doi:10.1103/PhysRevLett.110.021101. PMID 23679701.
4. ^ Steffen, Jason H.; Gammev Collaboration (2008). "Constraints on chameleons and axion-like particles from the GammeV experiment". Proceedings of "Identification of Dark Matter 2008". August 18-22, 2008, Stockholm, Sweden. p. 064. arXiv:0810.5070. Bibcode:2008idm..confE..64S.
5. ^ Rybka, G; Hotz, M; Rosenberg, L. J.; Asztalos, S. J.; Carosi, G; Hagmann, C; Kinion, D; Van Bibber, K; Hoskins, J; Martin, C; Sikivie, P; Tanner, D. B.; Bradley, R; Clarke, J (2010). "Search for chameleon scalar fields with the axion dark matter experiment". Physical Review Letters. 105 (5): 051801. arXiv:1004.5160. Bibcode:2010PhRvL.105a1801B. doi:10.1103/PhysRevLett.105.051801. PMID 20867906.
6. ^ GammeV experiment at Fermilab
7. ^ Chou, A. S.; Wester, W.; Baumbaugh, A.; Gustafson, H. R.; Irizarry-Valle, Y.; Mazur, P. O.; Steffen, J. H.; Tomlin, R.; Upadhye, A.; Weltman, A.; Yang, X.; Yoo, J. (22 Jan 2009). "Search for Chameleon Particles Using a Photon-Regeneration Technique". Physical Review Letters. 102 (3): 030402. arXiv:0806.2438. Bibcode:2009PhRvL.102c0402C. doi:10.1103/PhysRevLett.102.030402. PMID 19257328.
8. ^ Steffen, Jason H. (2010). "The CHASE laboratory search for chameleon dark energy". Proceedings of the 35th International Conference of High Energy Physics (ICHEP 2010). July 22-28, 2010. Paris, France. p. 446. arXiv:1011.3802. Bibcode:2010iche.confE.446S.
9. ^ Jenke, T.; Cronenberg, G.; Burgdörfer, J.; Chizhova, L. A.; Geltenbort, P.; Ivanov, A. N.; Lauer, T.; Lins, T.; Rotter, S.; Saul, H.; Schmidt, U.; Abele, H. (Apr 16, 2014). "Gravity Resonance Spectroscopy Constrains Dark Energy and Dark Matter Scenarios". Physical Review Letters. 112 (15): 151105. arXiv:1404.4099. Bibcode:2014PhRvL.112o1105J. doi:10.1103/PhysRevLett.112.151105. PMID 24785025.
10. ^ V. Anastassopoulos; M. Arik; S. Aune; K. Barth; A. Belov; H. Bräuninger; . . . K. Zioutas (March 16, 2015). "Search for chameleons with CAST". Physics Letters B. 749: 172–180. arXiv:1503.04561. Bibcode:2015PhLB..749..172A. doi:10.1016/j.physletb.2015.07.049.