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Frustrated expectations: Defect networks and dark energy

P. P. Avelino1,2,*, C. J. A. P. Martins1,3,†, J. Menezes1,‡, R. Menezes1,4,§, and J. C. R. E. Oliveira1,2,∥

  • 1Centro de Física do Porto, Rua do Campo Alegre 687, 4169-007 Porto, Portugal
  • 2Departamento de Física da Faculdade de Ciências da Universidade do Porto, Rua do Campo Alegre 687, 4169-007 Porto, Portugal
  • 3Department of Applied Mathematics and Theoretical Physics, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, United Kingdom
  • 4Departamento de Física, Universidade Federal da Paraíba, Caixa Postal 5008, 58051-970 João Pessoa, Paraíba, Brazil

  • *Electronic address: ppavelin@fc.up.pt
  • †Electronic address: C.J.A.P.Martins@damtp.cam.ac.uk
  • ‡Electronic address: jmenezes@fc.up.pt
  • §Electronic address: rms@fisica.ufpb.br
  • ∥Electronic address: jeolivei@fc.up.pt
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Phys. Rev. D 73, 123519 – Published 15 June, 2006

DOI: https://doi.org/10.1103/PhysRevD.73.123519

Abstract

We discuss necessary conditions for a network of cosmic domain walls to have a chance of providing the dark energy that might explain the recent acceleration of the Universe. We derive a strong bound on the curvature of the walls, which shows that viable candidate networks must be fine-tuned and nonstandard. We also discuss various requirements that any stable lattice of frustrated walls must obey. We conjecture that, even though one can build (by hand) lattices that would be stable, no such lattices will ever come out of realistic domain wall forming cosmological phase transitions. We provide some simple numerical simulations that illustrate our results and correct some misconceptions in the published literature, but a detailed numerical analysis is left for a companion paper.

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See Also

Defect junctions and domain wall dynamics

P. P. Avelino, C. J. A. P. Martins, J. Menezes, R. Menezes, and J. C. R. E. Oliveira
Phys. Rev. D 73, 123520 (2006)

Article Text

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Phys. Rev. D 73, 123519– Published 15 June, 2006
  • Received 27 February 2006

© 2006 American Physical Society

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