Cosmological Phase Transitions in a Brane World

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dc.creatorDavis, Stephen C.
dc.creatorPerkins, Warren B.
dc.creatorDavis, Anne-Christine
dc.creatorVernon, Ian R.
dc.date2000-12-18
dc.date2001-08-15
dc.date.accessioned2026-07-07T10:52:14Z
dc.date.available2026-07-07T10:52:14Z
dc.descriptionIn 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.
dc.descriptionRevTeX, 9 pages. This paper was previously part of hep-ph/0008132. v2: section 5 corrected
dc.identifierhttps://arxiv.org/abs/hep-ph/0012223
dc.identifierhttp://arxiv.org/abs/hep-ph/0012223
dc.identifierPhys.Rev.D63:083518,2001
dc.identifierdoi:10.1103/PhysRevD.63.083518
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/185088
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectHigh Energy Physics - Theory
dc.titleCosmological Phase Transitions in a Brane World
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