2007/02/20 by K. Koyama, Kazuya Koyama, Fábio Silva +1
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.75.084040
published as Phys.Rev.D75:084040,2007 · 11 pages
arxiv created 2007/02/20 · openalex publication_date 2007/04/27 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We study quasistatic perturbations in a cosmological background in the Dvali-Gabadadze-Porrati braneworld model. We identify the Vainshtein radius at which the nonlinear interactions of the brane bending mode become important in a cosmological background. The Vainshtein radius in the early universe is much smaller than the one in the Minkowski background, but in a self-accelerating universe it is the same as the Minkowski background. Our result shows that the perturbative approach is applicable beyond the Vainshtein radius for weak gravity by taking into account the second-order effects of the brane bending mode. The linearized cosmological perturbations are shown to be smoothly matched to the solutions inside the Vainshtein radius. We emphasize the importance of imposing a regularity condition in the bulk by solving the 5D perturbations and we highlight the problem of ad hoc assumptions on the bulk gravity that lead to different conclusions.