RT Journal Article
T1 Brane oscillations and the cosmic coincidence problem
A1 López Maroto, Antonio
AB We show that, under general assumptions, in six-dimensional brane-world models with compactified large extra dimensions, the energy density of brane oscillations scales as that of cold dark matter and its present value is compatible with observations. This value is obtained from the only dimensional scale in the theory, namely, the fundamental scale of gravity in six dimensions M(6)similar to1 TeV, without any fine-tuning or the introduction of additional mass scales apart from the large size of the extra dimensions. It has been suggested that the same kind of model could provide also the correct magnitude of the cosmological constant. This observation might be relevant for the resolution of the cosmic coincidence problem in the brane-world scenario.
PB American Physical Society
SN 0556-2821
YR 2004
FD 2004-05-24
LK https://hdl.handle.net/20.500.14352/51230
UL https://hdl.handle.net/20.500.14352/51230
LA eng
NO [1] D.N. Spergel et al., Astrophys. J., Suppl. Ser. 148, 175 (2003).[2] B. Ratra and P.J.E. Peebles, Phys. Rev. D 37, 3406 (1988); P.J.E. Peebles and B. Ratra, Rev. Mod. Phys. 75, 559 (2003); R.R. Caldwell, R. Dave, and P.J. Steinhardt, Phys. Rev. Lett. 80, 1582 (1998); I. Zlatev, L-M. Wang, and P.J. Steinhardt, ibid. 82, 896 (1999).[3] T. Chiba, T. Okabe, and M. Yamaguchi, Phys. Rev. D 62, 023511 (2000); C. Armendariz-Picon, V. Mukhanov, and P.J. Steinhardt, Phys. Rev. Lett. 85, 4438 (2000).[4] M. Malquarti, E.J. Copeland, and A.R. Liddle, Phys. Rev. D 68, 023512 (2003).[5] G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rep. 267, 195 (1996); C. Muñoz, hep-ph/0309346.[6] J.A. Frieman, C.T. Hill, A. Stebbins, and I. Waga, Phys. Rev. Lett. 75, 2077 (1995).[7] A. Albrecht, C.P. Burgess, F. Ravndal, and C. Skordis, Phys. Rev. D 65, 123507 (2002).[8] L. Perivolaropoulos and C. Sourdis, Phys. Rev. D 66, 084018 (2002).[9] R. Sundrum, Phys. Rev. D 59, 085010 (1999).[10] J.-W. Chen, M.A. Luty, and E. Ponton, J. High Energy Phys. 09, 012 (2000).[11] N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, Phys. Lett. B 429, 263 (1998); Phys. Rev. D 59, 086004 (1999); I. Antoniadis, Phys. Lett. B 246, 377 (1990).[12] P. Candelas and S. Weinberg, Nucl. Phys. B237, 397 (1984).[13] M. Pietroni, Phys. Rev. D 67, 103523 (2003).[14] M. Peloso and E. Poppitz, Phys. Rev. D 68, 125009 (2003).[15] Y. Aghababaie, C.P. Burgess, S.L. Parameswaran, and F. Quevedo, Nucl. Phys. B680, 389 (2004).[16] J.A.R. Cembranos, A. Dobado, and A.L. Maroto, Phys. Rev. Lett. 90, 241301 (2003).[17] A.L. Maroto, Phys. Rev. D 69, 043509 (2004).[18] R. Sundrum, Phys. Rev. D 59, 085009 (1999).[19] A. Dobado and A.L. Maroto, Nucl. Phys. B592, 203 (2001).[20] J. Alcaraz, J.A.R. Cembranos, A. Dobado, and A.L. Maroto, Phys. Rev. D 67, 075010 (2003).[21] J.A.R. Cembranos, A. Dobado, and A.L. Maroto, Phys. Rev. D 65, 026005 (2002).[22] J. Preskill, M.B. Wise, and F. Wilczek, Phys. Lett. 120B, 127 (1983); J.A. Frieman and A.H. Jaffe, Phys. Rev. D 45, 2674 (1992).[23] M.S. Turner, Phys. Rev. D 28, 1243 (1983).[24] J.A.R. Cembranos, A. Dobado, and A.L. Maroto, Phys. Rev. D 68, 103505 (2003).[25] F. Leblond, R.C. Myers, and D.J. Winters, J. High Energy Phys. 07, 031 (2001).[26] J.M. Cline, J. Descheneau, M. Giovannini, and J. Vinet, J. High Energy Phys. 06, 048 (2003).[27] P. Bostock, R. Gregory, I. Navarro, and J. Santiago, Phys. Rev. Lett. (to be published), hep-th/0311074.[28] T. Kugo and K. Yoshioka, Nucl. Phys. B594, 301 (2001).[29] P. Creminelli and A. Strumia, Nucl. Phys. B596, 125 (2001).[30] J.A.R. Cembranos, A. Dobado, and A.L. Maroto (in preparation).
NO © 2004 The American Physical Society. I would like to thank A. Dobado and J. A. R. Cembranos for useful comments. This work has been partially supported by the DGICYT (Spain) under Projects No. FPA 2000-0956 and No. BFM2002-01003.
NO DGICYT (Spain)
DS Docta Complutense
RD 30 abr 2024