2006/11/22 by L. Gazzola, E. J. King, F. R. Pearce +1 · 3 citations
Physics and Astronomy · #Astrophysics and Star Formation Studies #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2006.11323.x
published as Mon.Not.Roy.Astron.Soc.375:657-664,2007 · 9 pages, 9 figures. Accepted by MNRAS
arxiv created 2006/11/22 · openalex publication_date 2007/01/15 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We follow the growth of baryonic structure in the presence of a magnetic field within an approximate cosmological magneto-hydrodynamic simulation, produced by adding an (isotropic) magnetic pressure related to the local gas pressure. We perform an ensemble of these simulations to follow the amplification of the field with time. By using a variety of initial field strengths and changing the slope of the power law that governs the way the field grows with increasing density we span the range of current observations and demonstrate the size of the effect realistic magnetic fields could have on the central density of groups and clusters. A strong magnetic field significantly reduces the central gas density which, in turn, reduces observable quantities such as the X-ray luminosity.