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Inflation in the five-dimensional universe with an orbifold extra dimension

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arxiv hep-ph/9905487 v3 pith:HZQ7NMYG submitted 1999-05-26 hep-ph

classification hep-ph
keywords dimensionextrafive-dimensionalsolutionsbulkcosmologicalinflationorbifold
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abstract

New inflationary solutions to the Einstein equation are explicitly constructed in a simple five-dimensional model with an orbifold extra dimension $S^1/Z_2$. We consider inflation caused by cosmological constants for the five-dimensional bulk and the four-dimensional boundaries. In our solutions the extra dimension is static, and the background metric has a non-trivial configuration in the extra dimension. In addition to the solution for a vanishing bulk cosmological constant, which has already been discussed, we obtain solutions for a non-zero one.

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Suppressing Extra-Dimensional Axion Isocurvature Dynamically

    hep-ph 2026-07 conditional novelty 6.0 of 10

    Radion dynamics in warped 5D models enhance the axion decay constant during inflation, satisfying CMB isocurvature bounds at higher Hubble scales while restoring the QCD window afterward.

  2. Inflation with a Growing Fifth Dimension

    hep-th 2025-12 conditional novelty 6.0 of 10

    Inflation from a UV-brane inflaton in a warped 5D bulk with an IR brane predicts a blue-tilted low-k scalar spectrum and oscillating tensor features because the early adiabatic modes come from the radion.

  3. Quasinormal Ringing of de Sitter Braneworlds

    gr-qc 2024-12 conditional novelty 6.0 of 10

    Thin and thick de Sitter braneworlds have discrete, purely imaginary quasinormal frequencies for gravitational perturbations, with decay rates set by the Hubble constant and, for thick branes, by the brane width parameter.

  4. Analysis of inflationary models in higher-dimensional uniform inflation

    hep-ph 2025-01 conditional novelty 5.0 of 10

    In (D+4)-dimensional uniform inflation the spectral index and tensor-to-scalar ratio are ns=1-(D+6)ε+2η and r=8(D+2)ε, which excludes D≥2 for the five models studied while allowing D=1 in the b0k >> 1 branch.

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