Solitons and Universes with Acceleration Driven by Bulk Particles

Authors: A. C. Amaro de Faria Jr, A. M. Canone

Abstract:

Considering a scenario where our universe is taken as a 3d domain wall embedded in a 5d dimensional Minkowski space-time, we explore the existence of a richer class of solitonic solutions and their consequences for accelerating universes driven by collisions of bulk particle excitations with the walls. In particular it is shown that some of these solutions should play a fundamental role at the beginning of the expansion process. We present some of these solutions in cosmological scenarios that can be applied to models that describe the inflationary period of the Universe.

Keywords: Solitons, topological defects, Branes, kinks, accelerating universes in Brane scenarios.

References:

[1] F. A. Brito, F. F. Cruz and J. F. N. Oliveira, Phys. Rev. D 71, 083516 (2005).
[2] R. Rajaraman, Solitons and Instantons (North-Holand, Amsterdam, 1982)
[3] A. Vilenkin and E. P. S. Shellard, Cosmic Strings and Other Topological Defects (Cambridge University, Cambridge, England, 1994).
[4] T. Vachaspati, Kinks and Domain Walls: An Introduction to Classical and Quantum Solitons (Cambridge University Press, Cambrifge, England, 2006).
[5] D.Walgraef, Spatio-Temporal Pattern Formation (Springer-Verlag, Berlin, 1997).
[6] R. Rajaraman, Phys. Rev. Lett. 42, 200 (1979).
[7] R. Rajaraman an E. J. Weinberg, Phys. Rev. D 11, 2950 (1975).
[8] D. Bazeia, M. J. dos Santos and R. F. Ribeiro, Phys. Lett. A 208 (1995) 84. D. Bazeia, W. Freire, L. Losano and R. F. Ribeiro, Mod. Phys. Lett. A 17, 1945 (2002).
[9] M. K. Prasad and C. M. Sommerfeld, Phys. Rev. Lett. 35, 760 (1975); E. B. Bolgomol’nyi, Sov. J. Nucl. Phys. 24, 449 (1976).
[10] A. de Souza Dutra, Phys. Lett. B 626, 249 (2005).
[11] A. de Souza Dutra and A. C. F. de Amaral Jr., Phys.Lett. B 642 (2006) 274.
[12] D. Bazeia, J. R. S. Nascimento, R. F. Ribeiro and D. Toledo, J. Phys. A 30, 8157 (1997)
[13] D. Bazeia, Braz. J. Phys. 32 (2002) 869.
[14] M. N. Barreto, D. Bazeia and R. Menezes, Phys. Rev. D 73, 065015 (2006).
[15] A. de Souza Dutra, M. Hott and F.A. Barone, Phys. Rev. D 74, 085030 (2006).
[16] N. Arkani-Hamed, S. Dimopoulos and G. R. Dvali, Phys. Lett. B 429 (1998) 263.
[17] L. Randall and R. Sundrum, Phys. Rev. Lett. 83 (1999) 4690.
[18] G. Dvali, G. Gabadadze and M. Porrati, Phys. Lett. B 485 (2000) 208.
[19] G. Dvali and G. Gabadadze, Phys. Rev. D 63 (2001) 065007.
[20] P. S. Apostopoulos and N. Tetradis, Phys. Rev. D 71 (2005) 043506.
[21] P. S. Apostopoulos and N. Tetradis, Phys. Lett. B 633 (2006) 409.
[22] C. Bogdanos and K. Tamvakis, Phys. Lett. B 646 (2007) 39.
[23] M. A. Shiffman and M. B. Voloshin, Phys. Rev. D 57 (1998) 2590.
[24] L. J. Boya and J. Casahorran, Phys. Rev. A 39, 4298 (1989).
[25] A. G. Riess, et al., Astron. J. 116 (1998) 1009. S. Perlmutter, et al., Astron. J. 517 (1999) 565. A. G. Riess, et al., Astron. J. 607 (2004) 665.