2006/11/30 by Dai Yamazaki, Dai G. Yamazaki, Kiyotomo Ichiki +3 · 36 citations
Physics and Astronomy · #Amplitude #Astrophysics #Cosmology and Gravitation Theories #Field (mathematics) #Galaxies: Formation, Evolution, Phenomena #Lambda #Magnetic field #Physics #Quantum mechanics #Spectral index #Spectral line #Stellar, planetary, and galactic studies #Universe #astro-ph #gr-qc
paper · pdf · doi:10.1103/physrevd.74.123518
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 74(12) (American Physical Society) · 20 pages, 5 figures, submitted to PRD 23 Jan 2006, Revised 02 Oct 2006, accepted for publication in PRD
arxiv created 2006/12/01 · openalex publication_date 2006/12/22 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Magnetic field plays a very important role in many astronomical phenomena at various scales of the universe. It is no exception in the early universe. Since the energy density, pressure, and tension of the primordial magnetic field affect gravitational collapses of plasma, the formation of seeds for large-scale structures should be influenced by them. Here we numerically investigate the effects of stochastic primordial magnetic field on the seeds of large-scale structures in the universe in detail. We found that the amplitude ratio between the density spectra with and without PMF (|P(k)/P0(k)| at k>0.2 Mpc^\ensuremath-1) lies between 75% and 130% at present for the range of PMF strengths 0.5nG<B_\ensuremathλ<1.0nG, depending on the spectral index of PMF and the correlation between the matter density and the PMF distributions.