The Co-Evolution of a Magnetized Intracluster Medium and Hot Galactic Coronae: Magnetic Field Amplification and Turbulence Generation

Abstract

We use adaptive-mesh magnetohydrodynamic simulations to study the effect of magnetic fields on ram pressure stripping of galaxies in the intracluster medium (ICM). Although the magnetic pressure in typical clusters is not strong enough to affect the gas mass loss rate from galaxies, magnetic fields can affect the morphology of stripped galaxies. ICM magnetic fields are draped around orbiting galaxies and aligned with their stripped tails. Magnetic fields suppress shear instabilities at the galaxy-ICM interface, and magnetized tails are smoother and narrower than tails in comparable hydrodynamic simulations in Vijayaraghavan & Ricker (2015). Orbiting galaxies stretch and amplify ICM magnetic fields, amplifying magnetic power spectra on $10-100$ kpc scales. Galaxies inject turbulent kinetic energy into the ICM via their turbulent wakes and $g$-waves. The magnetic energy and kinetic energy in the ICM increase up to $1.5-2$ Gyr of evolution, after which galaxies are stripped of most of their gas, and do not have sufficiently large gaseous cross sections to further amplify magnetic fields and inject turbulent kinetic energy. The increase in turbulent pressure due to galaxy stripping and generation of $g$-waves results in an increase in the turbulent volume fraction of the ICM. This turbulent kinetic energy is not a significant contributor to the overall ICM energy budget, but greatly impacts the evolution of the ICM magnetic field. Additionally, the effect of galaxies on magnetic fields can potentially be observed in high resolution Faraday rotation measure (RM) maps as small scale fluctuations in the RM structure.

26 pages, 23 figures, accepted for publication in ApJ. This paper has been updated to reflect the version accepted for publication

References in corpus (29)

• Properties of galaxies reproduced by a hydrodynamic simulation
• Testing X-ray Measurements of Galaxy Clusters with Cosmological Simulations
• The Quiescent Intracluster Medium in the Core of the Perseus Cluster
• Rotation-Dependent Catastrophic Disruption of Gravitational Aggregates
• Draping of Cluster Magnetic Fields over Bullets and Bubbles -- Morphology and Dynamic Effects
• Cosmology and Astrophysics from Relaxed Galaxy Clusters II: Cosmological Constraints
• Splashback in accreting dark matter halos
• Hydrodynamic Simulation of Non-thermal Pressure Profiles of Galaxy Clusters
• Cluster Magnetic Fields from Galactic Outflows
• X-ray thermal coronae of galaxies in hot clusters -- ubiquity of embedded mini cooling cores
• Magnetic draping of merging cores and radio bubbles in clusters of galaxies
• A Direct Multigrid Poisson Solver for Oct-Tree Adaptive Meshes
• On the amplification of magnetic fields in cosmic filaments and galaxy clusters
• Impact of tangled magnetic fields on AGN-blown bubbles
• The relation between gas density and velocity power spectra in galaxy clusters: high-resolution hydrodynamic simulations and the role of conduction
• Cosmological MHD simulation of a cooling flow cluster
• Hydrodynamical adaptive mesh refinement simulations of turbulent flows - II. Cosmological simulations of galaxy clusters
• The Matryoshka Run (II): Time Dependent Turbulence Statistics, Stochastic Particle Acceleration and Microphysics Impact in a Massive Galaxy Cluster
• Stripped elliptical galaxies as probes of ICM physics: II. Stirred, but mixed? Viscous and inviscid gas stripping of the Virgo elliptical M89
• Thermal Balance in the Intracluster Medium: Is AGN Feedback Necessary?
• Stripped elliptical galaxies as probes of ICM physics: I. Tails, wakes, and flow patterns in and around stripped ellipticals
• The Ties that Bind? Galactic Magnetic Fields and Ram Pressure Stripping
• Magnetic field amplification by shocks in galaxy clusters: application to radio relics
• The ASTRO-H X-ray Astronomy Satellite
• Bubble-Wrap for Bullets: The Stability Imparted By A Thin Magnetic Layer
• Ram Pressure Stripping of Hot Coronal Gas from Group and Cluster Galaxies and the Detectability of Surviving X-ray Coronae
• Heating and Turbulence Driving by Galaxy Motions in Galaxy Clusters
• N-body + Magnetohydrodynamical Simulations of Merging Clusters of Galaxies: Characteristic Magnetic Field Structures Generated by Bulk Flow Motion
• Ram pressure stripping in elliptical galaxies: II. magnetic field effects

Cited by in corpus (11)

• Ram Pressure Stripping in High-Density Environments
• Interaction of a cold cloud with a hot wind: the regimes of cloud growth and destruction and the impact of magnetic fields
• LoTSS jellyfish galaxies: I. Radio tails in low redshift clusters
• Galaxy formation with L-GALAXIES: Modelling the environmental dependency of galaxy evolution and comparing with observations
• Highly ordered magnetic fields in the tail of the jellyfish galaxy JO206
• A New Method to Quantify Environment and Model Ram-Pressure Stripping in N-Body Simulations
• A Parameter Space Exploration of Galaxy Cluster Mergers II: Effects of Magnetic Fields
• Turbulent magnetic fields in merging clusters: A case study of Abell 2146
• The Evaporation and Survival of Cluster Galaxies' Coronae Part II: The Effectiveness of Anisotropic Thermal Conduction and Survival of Stripped Galactic Tails
• Implications of the mild gas motion found with Hitomi in the core of the Perseus cluster
• A Lack of Evidence for Global Ram-pressure Induced Star Formation in the Merging Cluster Abell 3266