2007/12/31 by Kenji Tomita, Kaiki Taro Inoue · 1 citation
Physics and Astronomy · #Anisotropy #Astrophysics #Black Holes and Theoretical Physics #Cosmic microwave background #Cosmology #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gravitation #Gravitational potential #Isotropy #Lambda #Mathematical physics #Order (exchange) #Perturbation (astronomy) #Physics #Planck #Quantum mechanics #Redshift #Shape of the universe #astro-ph #gr-qc
paper · pdf · doi:10.1103/physrevd.77.103522
published as Phys.Rev.D77:103522,2008 · 16 pages, 8 figures, No major change. Eqs (5.6) and (5.7) are modified to include uncompensating cases
arxiv created 2008/05/15 · openalex publication_date 2008/05/27 · arxiv updated 2014/09/08 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We study second order gravitational effects of local inhomogeneities on the cosmic microwave background radiation in flat universes with matter and a cosmological constant \ensuremathΛ. We find that the general relativistic correction to the Newtonian approximation is negligible at second order provided that the size of the inhomogeneous region is sufficiently smaller than the horizon scale. For a spherically symmetric top-hat type quasilinear perturbation, the first order temperature fluctuation corresponding to the linear integrated Sachs-Wolfe effect is enhanced (suppressed) by the second order one for a compensated void (lump). As a function of redshift of the local inhomogeneity, the second order temperature fluctuations due to evolution of the gravitational potential have a peak before the matter-\ensuremathΛ equality epoch for a fixed comoving size and a density contrast. The second order gravitational effects from local quasilinear inhomogeneities at a redshift z\ensuremath∼1 may significantly affect the cosmic microwave background.