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Publisher: American Physical Society
Languages: English
Types: Article
Subjects: General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory, Astrophysics - Cosmology and Nongalactic Astrophysics
We describe a symmetron model in which the screening of fifth forces arises at the one-loop level through the Coleman-Weinberg mechanism of spontaneous symmetry breaking. We show that such a theory can avoid current constraints on the existence of fifth forces but still has the potential to give rise to observable deviations from general relativity, which could be seen in cold atom experiments.
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    • ‡ [1] E. J. Copeland, M. Sami, and S. Tsujikawa, Int. J. Mod.
    • Phys. D 15, 1753 (2006). [2] T. Clifton, P. G. Ferreira, A. Padilla, and C. Skordis, Phys.
    • Rep. 513, 1 (2012). [3] L. Amendola (Euclid Theory Working Group), Living Rev.
    • Relativ. 16, 6 (2013). [4] B. Jain, V. Vikram, and J. Sakstein, Astrophys. J. 779, 39
    • (2013). [5] P. Hamilton, M. Jaffe, P. Haslinger, Q. Simmons, H. Müller,
    • and J. Khoury, Science 349, 849 (2015). [6] Ph. Brax and A. C. Davis, arXiv:1609.09242. [7] C. Burrage, A. Kuribayashi-Coleman, J. Stevenson, and B.
    • Thrussell, arXiv:1609.09275. [8] V. Anastassopoulos et al. (CAST Collaboration), Phys. Lett.
    • B 749, 172 (2015). [9] A. Joyce, B. Jain, J. Khoury, and M. Trodden, Phys. Rep.
    • 568, 1 (2015). [10] K. Hinterbichler and J. Khoury, Phys. Rev. Lett. 104,
    • 231301 (2010). [11] K. Hinterbichler, J. Khoury, A. Levy, and A. Matas, Phys.
    • Rev. D 84, 103521 (2011). [12] M. Pietroni, Phys. Rev. D 72, 043535 (2005). [13] K. A. Olive and M. Pospelov, Phys. Rev. D 77, 043524
    • (2008). [14] T. Damour and A. M. Polyakov, Nucl. Phys. B423, 532 (1994). [15] Ph. Brax, C. van de Bruck, A. C. Davis, B. Li, and D. J.
    • Shaw, Phys. Rev. D 83, 104026 (2011). [16] Reference [17] considers an alternative region of parameter
    • space with μ ∼ 10−3 eV. Measurements made by the
    • Eöt-Wash experiment then force M ≲ 10 GeV if λ ≲ 1. [17] A. Upadhye, Phys. Rev. Lett. 110, 031301 (2013). [18] S. R. Coleman and E. J. Weinberg, Phys. Rev. D 7, 1888
    • (1973). [19] We employ the ð−; −; −Þ sign convention established in
    • (W. H. Freeman, San Francisco, 1973). [20] R. Jackiw, Phys. Rev. D 9, 1686 (1974). [21] Here, since we do not consider the loop corrections to the
    • energy-momentum tensor, we do not include the OðR2Þ
    • counterterms that would otherwise be necessary. [22] B. Garbrecht and P. Millington, Phys. Rev. D 92, 125022
    • (2015). [23] Note that we must first vary with respect to φ, keeping the
    • equation from Eq. (19). [24] M. E. Carrington, Phys. Rev. D 45, 2933 (1992). [25] A. D. Linde, Phys. Lett. 100B, 37 (1981); Nucl. Phys. B216,
    • 421 (1983); B223, 544(E) (1983). [26] E. Witten, Phys. Rev. D 30, 272 (1984). [27] A. Kosowsky, M. S. Turner, and R. Watkins, Phys. Rev. D
    • 45, 4514 (1992). [28] C. Caprini, R. Durrer, T. Konstandin, and G. Servant, Phys.
    • Rev. D 79, 083519 (2009). [29] R. Hempfling, Phys. Lett. B 379, 153 (1996). [30] W. F. Chang, J. N. Ng, and J. M. S. Wu, Phys. Rev. D 75,
    • 115016 (2007). [31] C. Englert, J. Jaeckel, V. V. Khoze, and M. Spannowsky,
    • J. High Energy Phys. 04 (2013) 060. [32] Ph. Brax, C. van de Bruck, A. C. Davis, D. J. Shaw, and D.
    • Iannuzzi, Phys. Rev. Lett. 104, 241101 (2010). [33] Ph. Brax and G. Pignol, Phys. Rev. Lett. 107, 111301
    • (2011). [34] A. Upadhye, Phys. Rev. D 86, 102003 (2012). [35] T. Jenke et al., Phys. Rev. Lett. 112, 151105 (2014). [36] H. Lemmel, Ph. Brax, A. N. Ivanov, T. Jenke, G. Pignol, M.
    • H. Abele, Phys. Lett. B 743, 310 (2015). [37] K. Li et al., Phys. Rev. D 93, 062001 (2016). [38] A. D. Rider, D. C. Moore, C. P. Blakemore, M. Louis, M.
    • Lu, and G. Gratta, Phys. Rev. Lett. 117, 101101 (2016). [39] C. Caprini, R. Durrer, and X. Siemens, Phys. Rev. D 82,
    • 063511 (2010). [40] C. Caprini, M. Hindmarsh, S. Huber, T. Konstandin, J.
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