1998/11/30 by Nemanja Kaloper, Andrei Linde · 5 citations
Mathematics · Physics and Astronomy · #Astrophysics #Black Holes and Theoretical Physics #Compactification (mathematics) #Computer science #Cosmology #Cosmology and Gravitation Theories #Flatness (cosmology) #Inflation (cosmology) #Inflaton #Mathematics #Particle physics theoretical and experimental studies #Physics #Pure mathematics #Quantum mechanics #Scale (ratio) #Theoretical physics #Unification #astro-ph #gr-qc #hep-ph #hep-th
paper · pdf · doi:10.1103/physrevd.59.101303
published as Phys.Rev.D59:101303,1999 · 4 pages, revtex, minor modifications
arxiv created 1998/12/12 · openalex publication_date 1999/04/06 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We consider some aspects of inflation in models with large internal dimensions. If inflation occurs on a 3D wall after the stabilization of internal dimensions in the models with low unification scale (M\ensuremath∼1 TeV), the inflaton field must be extremely light. This problem may disappear in models with an intermediate (M\ensuremath∼1011 GeV) to high (M\ensuremath∼1016 GeV) unification scale. However, in all of these cases the wall inflation does not provide a complete solution to the horizon and flatness problems. To solve them, there must be a stage of inflation in the bulk before the compactification of internal dimensions.