Publication: Dark matter clues in the muon anomalous magnetic moment
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2006-03
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American Physical Society
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Abstract
We study the possibility to explain the nonbaryonic dark matter abundance and improve the present fits on the muon anomalous magnetic moment through the same new physics. In this work we show that massive brane fluctuations (branons) in large extra-dimensions models can provide an economical way to deal with these two issues. This is so because the low-energy branon physics depends effectively on essentially only three parameters. Next collider experiments, such as LHC or ILC, will be sensitive to branon phenomenology in the natural parameter region where the theory is able to account for the two effects.
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© 2006 The American Physical Society.
This work is partially supported by DGICYT (Spain)
under project numbers FPA 2004-02602 and BFM 2002-
01003, by NSF grant No. PHY-0239817 and by the
Fulbright-MEC (Spain) program.
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[1] D. N. Spergel et al., Astrophys. J. Suppl. Ser. 148, 175 (2003).
[2] G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rep. 267, 195 (1996).
[3] H. C. Cheng, J. L. Feng, and K. T. Matchev, Phys. Rev. Lett. 89, 211301 (2002); G. Servant and T. M. P. Tait, Nucl. Phys. B650, 391 (2003).
[4] M. Perelstein, hep-ph/0512128.
[5] S. Eidelman et al., Phys. Lett. B 592, 1 (2004).
[6] T. Kinoshita and M. Nio, Phys. Rev. D 73, 013003 (2006).
[7] H. N. Brown et al., Phys. Rev. Lett. 86, 2227 (2001); G. W. Bennett et al., Phys. Rev. Lett. 89, 101804 (2002); 92, 161802 ( 2004).
[8] M. Passera, J. Phys. G 31, R75 (2005); J. F. de Troconiz and F. J. Yndurain,Phys. Rev. D 71, 073008 (2005); A. Hocker, hep-ph/0410081.
[9] N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, Phys. Lett. B 429, 263 (1998); Phys. Rev. D 59, 086004 (1999); I. Antoniadis et al., Phys. Lett. B 436, 257 (1998).
[10] J. A. R. Cembranos, A. Dobado, and A. L. Maroto, Phys. Rev. Lett. 90, 241301 (2003).
[11] A. L. Maroto, Phys. Rev. D 69, 043509 (2004); 69, 101304 (2004); J. A. R. Cembranos, A. Dobado, and A. L. Maroto, Int. J. Mod. Phys. D 13, 2275 (2004); hep-ph/0402142; hep-ph/0406076; eConf C041213, 1113 (2004); hep-ph/ 0411076; astro-ph/0411262; astro-ph/0512569; .AMS Internal Note 2003-08-02.
[12] R. Sundrum, Phys. Rev. D 59, 085009 (1999); A. Dobado and A. L. Maroto Nucl. Phys. B592, 203 (2001).
[13] M. Bando et al., Phys. Rev. Lett. 83, 3601 (1999).
[14] J. A. R. Cembranos, A. Dobado, and A. L. Maroto, Phys. Rev. D 65, 026005 (2002); hep-ph/0107155.
[15] J. Alcaraz et al., Phys. Rev. D 67, 075010 (2003); J. A. R. Cembranos, A. Dobado, and A. L. Maroto, Phys. Rev. D 70, 096001 (2004); hep-ph/0307015; AIP Conf. Proc. No. 670 (AIP, New York, 2003); hep-ph/0511332; hepph/0512302; P. Achard et al., Phys. Lett. B 597, 145 (2004).
[16] P. Creminelli and A. Strumia, Nucl. Phys. B596, 125 (2001).
[17] J. A. R. Cembranos, A. Dobado, and A. L. Maroto, Phys. Rev. D 68, 103505 (2003); T. Kugo and K. Yoshioka, Nucl. Phys. B594, 301 (2001).
[18] J. A. R. Cembranos, A. Dobado, and A. L. Maroto, hep-ph/0510399.
[19] M. L. Graesser, Phys. Rev. D 61, 074019 (2000); S. C. Park and H. S. Song, Phys. Lett. B 523, 161 (2001); K. Sawa, Phys. Rev. D 73, 025010 (2006).
[20] R. Contino, L. Pilo, R. Rattazzi, and A. Strumia, J. High Energy Phys. 06 (2001) 005.
[21] G. Giudice and A. Strumia, Nucl. Phys. V663, 377 (2003).
[22] J. L. Hewett, Phys. Rev. Lett. 82, 4765 (1999).
[23] C. Adloff et al., Phys. Lett. B 568, 35 (2003).
[24] B. Abbott et al., Phys. Rev. Lett. 86, 1156 (2001).
[25] D. Abbaneo et al., hep-ex/0412015.
[26] M. E. Peskin and T. Takeuchi, Phys. Rev. D 46, 381 (1992).
[27] G. Altarelli, R. Barbieri, and F. Caravaglios, Int. J. Mod. Phys. A 13, 1031 (1998).
[28] G. Altarelli, hep-ph/0406270.
[29] A. Dobado, A. Go´mez-Nicola, A. L. Maroto, and J. R. Pela´ ez, Effective Lagrangians for the Standard Model (Springer-Verlag, Berlin, 1997).