Cosmological Phase Transitions in a Brane World

Details Cosmological Phase Transitions in a Brane World Cosmological Phase Transitions in a Brane World

2000-12-18

arxiv.org/abs/hep-ph/0012223v2

Phys.Rev.D63:083518,2001

Physics

High Energy Physics

High Energy Physics - Phenomenology

RevTeX, 9 pages. This paper was previously part of hep-ph/0008132. v2: section 5 corrected

Scientific paper

10.1103/PhysRevD.63.083518

In brane world scenarios the Friedmann equation is modified, resulting in an increased expansion at early times. This has important effects on cosmological phase transitions which we investigate, elucidating significant differences to the standard case. First order phase transitions require a higher nucleation rate to complete; baryogenesis and particle abundances could be suppressed. Topological defect evolution is also affected, though the current defect densities are largely unchanged. In particular, the increased expansion does not solve the usual monopole and domain wall problems.

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