Origin of Magnetic Field in the Intracluster Medium: Primordial or Astrophysical?

Abstract

The origin of magnetic fields in clusters of galaxies is still an unsolved problem, which is largely due to our poor understanding of initial seed magnetic fields. If the seed magnetic fields have primordial origins, it is likely that large-scale pervasive magnetic fields were present before the formation of the large-scale structure. On the other hand, if they were ejected from astrophysical bodies, they were highly localized in space at the time of injection. In this paper, using turbulence dynamo models for high magnetic Prandtl number fluids, we find constraints on the seed magnetic fields. The hydrodynamic Reynolds number based on the Spitzer viscosity in the intracluster medium (ICM) is believed to be less than $O(10^2)$, while the magnetic Reynolds number can be much larger than that. In this case, if the seed magnetic fields have primordial origins, they should be stronger than $O(10^{-11})$G, which is very close to the upper limit of $O(10^{-9})$G set by the cosmic microwave background (CMB) observations. On the other hand, if the seed magnetic fields were ejected from astrophysical bodies, any seed magnetic fields stronger than $O(10^{-9})$G can safely magnetize the intracluster medium. Therefore, it is less likely that primordial magnetic fields are the direct origin of present-day magnetic fields in the ICM.

arXiv comment11 pages, 10 figures, Accepted for publication in the ApJ

References in corpus (40)

• Astrophysical magnetic fields and nonlinear dynamo theory
• Origin of Galactic and Extragalactic Magnetic Fields
• Cosmological Magnetic Fields: Their Generation, Evolution and Observation
• Cluster Magnetic Fields
• Simulations of small-scale turbulent dynamo
• Magnetic Field in Clusters of Galaxies
• The Protogalactic Origin for Cosmic Magnetic Fields
• Turbulence and Magnetic Fields in the Large Scale Structure of the Universe
• On the Origin of Cosmic Magnetic Fields
• Compressible Turbulence in Galaxy Clusters: Physics and Stochastic Particle Re-acceleration
• Observations of extended radio emission in clusters
• The Evolution of Cosmic Magnetic Fields: From the Very Early Universe, to Recombination, to the Present
• Evolving turbulence and magnetic fields in galaxy clusters
• A Bayesian view on Faraday rotation maps - Seeing the magnetic power spectra in galaxy clusters
• The First Magnetic Fields
• The generation of strong magnetic fields during the formation of the first stars
• Cluster Heating by Viscous Dissipation of Sound Waves
• Small-scale dynamo action during the formation of the first stars and galaxies. I. The ideal MHD limit
• Turbulence, magnetic fields and plasma physics in clusters of galaxies
• Massive and Refined. II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution
• Current status of turbulent dynamo theory: From large-scale to small-scale dynamos
• Magnetic Field Evolution in Merging Clusters of Galaxies
• Cluster Magnetic Fields from Galactic Outflows
• Magnetic Energy of the Intergalactic Medium from Galactic Black Holes
• Magnetic fields in the Large-Scale Structure of the Universe
• The Small-Scale Dynamo and Non-Ideal MHD in Primordial Star Formation
• Growth of Magnetic Fields Induced by Turbulent Motions
• The Generation of Magnetic Fields Through Driven Turbulence
• Morphology of Rising Hydrodynamic and Magneto-hydrodynamic Bubbles from Numerical Simulations
• Cosmic magnetization: from spontaneously emitted aperiodic turbulent to ordered equipartition fields
• The Matryoshka Run: Eulerian Refinement Strategy to Study Statistics of Turbulence in Virialized Cosmic Structures
• Magnetic field amplification by shocks in galaxy clusters: application to radio relics
• Evolution and Distribution of Magnetic Fields from AGNs in Galaxy Clusters. I. The Effect of Injection Energy and Redshift
• Turbulent magnetic field amplification from the smallest to the largest magnetic Prandtl numbers
• Magnetic field amplification by the small-scale dynamo in the early Universe
• Effects of multiple-scale driving on turbulence statistics
• Magnetic fields during high redshift structure formation
• Dispersal of Galactic Magnetic Fields into Intracluster Space
• Growth of a localized seed magnetic field in a turbulent medium
• Fast Diffusion of Magnetic Field in Turbulence and Origin of Cosmic Magnetism

Cited by in corpus (29)

• Resolved magnetic dynamo action in the simulated intracluster medium
• Simulations of extragalactic magnetic fields and of their observables
• Vorticity, Shocks and Magnetic Fields in Subsonic, ICM-like Turbulence
• The large-scale properties of simulated cosmological magnetic fields
• Dynamical evolution of magnetic fields in the intracluster medium
• Fast magnetic field amplification in distant galaxyclusters
• Magnetic fields and relativistic electrons fill entire galaxy cluster
• Seed magnetic fields in turbulent small-scale dynamos
• Magnetogenesis around the first galaxies: the impact of different field seeding processes on galaxy formation
• Curved Radio Spectra of Weak Cluster Shocks
• Detecting shocked intergalactic gas with X-ray and radio observations
• Evolution of primordial magnetic fields during large-scale structure formation
• Multi-scale analysis of turbulence evolution in the density stratified intracluster medium
• Simulations and observational tests of primordial magnetic fields from Cosmic Microwave Background constraints
• The evolution of primordial magnetic field since its generation
• Viscosity, pressure, and support of the gas in simulations of merging cool-core clusters
• Troubled cosmic flows: turbulence, enstrophy and helicity from the assembly history of the intracluster medium
• Connecting turbulent velocities and magnetic fields in galaxy cluster simulations with active galactic nuclei jets
• Dynamical heating of the X-ray emitting intracluster medium: the roles of merger shocks and turbulence dissipation
• A nonlinear structural subgrid-scale closure for compressible MHD Part I: derivation and energy dissipation properties
• Fast magnetic field amplification in the early Universe: growth of collisionless plasma instabilities in turbulent media
• On the nature of LOFAR RMs and new constraints on magnetic fields in cosmic filaments and on magnetogenesis scenarios
• Limits and challenges of the detection of cluster-scale diffuse radio emission at high redshift: The Massive and Distant Clusters of WISE Survey (MaDCoWS) in LoTSS-DR2
• Generation of Solenoidal Modes and Magnetic Fields in Turbulence Driven by Compressive Driving
• Galactic winds and the origin of large-scale magnetic fields
• Radio Observations as a Probe of Cosmic Web Magnetism
• On the interpretation of XRISM X-ray measurements of turbulence in the intracluster medium: a comparison with cosmological simulations
• Effective Viscosity in the Intracluster Medium During Magnetic Field Amplification via Turbulent Dynamo
• Introduction to Strong Alfvénic MHD Turbulence