The Growth of Baryonic Structure in the Presence of Cosmological Magnetic Pressure

Abstract

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.

arXiv comment9 pages, 9 figures. Accepted by MNRAS

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Cited by in corpus (5)

• Resolved magnetic dynamo action in the simulated intracluster medium
• On the amplification of magnetic fields in cosmic filaments and galaxy clusters
• Non-thermal processes in cosmological simulations
• Investigating the influence of magnetic fields upon structure formation with AMIGA - a C code for cosmological magnetohydrodynamics
• The tension of cosmological magnetic fields as a contribution to dark energy