Turbulent Magnetic Field Amplification by the Interaction of Shock Wave and Inhomogeneous Medium

Abstract

Magnetic fields on the order of 100 $\mu$G observed in young supernova remnants cannot be amplified by shock compression alone. To investigate the amplification caused by turbulent dynamo, we perform three-dimensional MHD simulations of the interaction between shock wave and inhomogeneous density distribution with a shallow spectrum in the preshock medium. The postshock turbulence is mainly driven by the strongest preshock density contrast and follows the Kolmogorov scaling. The resulting turbulence amplifies the postshock magnetic field. The time evolution of the magnetic fields agrees with the prediction of the nonlinear turbulent dynamo theory in Xu & Lazarian (2016). When the initial weak magnetic field is perpendicular to the shock normal, the maximum amplification of the field's strength achieves a factor of $\approx 200$, which is twice larger than that for a parallel shock. We find that the perpendicular shock exhibits a smaller turbulent Alfvén Mach number in the vicinity of the shock front than the parallel shock. However, the strongest magnetic field has a low volume filling factor and is limited by the turbulent energy due to the reconnection diffusion taking place in a turbulent and magnetized fluid. The magnetic field strength averaged along the $z$-axis is reduced by a factor $\gtrsim 10$. We decompose the turbulent velocity and magnetic field into solenoidal and compressive modes. The solenoidal mode is dominant and evolves to follow the Kolmogorov scaling, even though the preshock density distribution has a shallow spectrum. When the preshock density distribution has a Kolmogorov spectrum, the turbulent velocity's compressive component increases.

arXiv comment19 pages, 15 figures, accepted for publication in ApJ

References in corpus (58)

• Theory of Star Formation
• Control of star formation by supersonic turbulence
• Astrophysical magnetic fields and nonlinear dynamo theory
• Reconnection in a Weakly Stochastic Field
• The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers
• Turbulent molecular clouds
• The Cassiopeia A Supernova was of Type IIB
• Fine Structures of Shock of SN 1006 with the Chandra Observation
• Density Fluctuations in MHD Turbulence: Spectra, Intermittency and Topology
• Toward Understanding the Cosmic-ray Acceleration at Young Supernova Remnants Interacting with Interstellar Clouds: Possible Applications to RX J1713.7-3946
• Extending Big Power Law in the Sky with Turbulence Spectra from WHAM data
• Turbulence and Magnetic Field Amplification in Supernova Remnants: Interactions Between A Strong Shock Wave and Multi-Phase Interstellar Medium
• Confirmation of strong magnetic field amplification and nuclear cosmic ray acceleration in SN 1006
• Velocity Modification of Power Spectrum from Absorbing Medium
• Turbulence-induced magnetic fields and the structure of Cosmic Ray modified shocks
• Mapping the X-ray Emitting Ejecta in Cassiopeia A with Chandra
• Growth of Magnetic Fields Induced by Turbulent Motions
• Studying Turbulence using Doppler-broadened lines: Velocity Coordinate Spectrum
• Superdiffusion of Cosmic Rays: Implications for Cosmic Ray Acceleration
• The Generation and Dissipation of Interstellar Turbulence - Results from Large Scale High Resolution Simulations
• Power Spectrum of the density of cold atomic gas in the Galaxy towards Cas A and Cygnus A
• Proper Motions and Brightness Variations of Nonthermal X-ray Filaments in the Cassiopeia A Supernova Remnant
• Obtaining Spectra of Turbulent Velocity from Observations
• Cosmic Ray Parallel and Perpendicular Transport in Turbulent Magnetic Fields
• Universal behaviour of shock precursors in the presence of efficient cosmic-ray acceleration
• On the Amplification of Magnetic Field by a Supernova Blast Shock Wave in a Turbulent Medium
• Turbulent dynamo in a conducting fluid and partially ionized gas
• Magnetic Field Morphology in Interstellar Clouds with the Velocity Gradient Technique
• Origin of Radially Aligned Magnetic Fields in Young Supernova Remnants
• Distribution of velocity gradient orientations: Mapping magnetization with the Velocity Gradient Technique
• Turbulent magnetic field amplification driven by cosmic-ray pressure gradients
• Magnetic Field Amplification and Saturation in Turbulence Behind a Relativistic Shock
• Cosmic ray diffusion near the Bohm limit in the Cassiopeia A supernova remnant
• On magnetic field amplification and particle acceleration near non-relativistic astrophysical shocks: Particles in MHD Cells simulations
• Amplification of Interstellar Magnetic Fields and Turbulent Mixing by Supernova-Driven Turbulence Part II - The Role of Dynamical Chaos
• Turbulent amplification of magnetic field driven by dynamo effect at rippled shocks
• Superdiffusion of Cosmic Rays in Compressible Magnetized Turbulence
• Magnetic Fields in the Formation of the First Stars. I. Theory vs. Simulation
• Magnetic-Field Amplification in the Thin X-ray Rims of SN1006
• Star formation from dense shocked regions in supersonic isothermal magneto-turbulence
• The Multi-phase Turbulence Density Power Spectra in the Perseus Molecular Cloud
• The Efficiency of Magnetic Field Amplification at Shocks by Turbulence
• Adiabatic non-resonant acceleration in magnetic turbulence and hard spectra of gamma-ray bursts
• Revealing Gravitational Collapse in Serpens G3-G6 Molecular Cloud using Velocity Gradients
• Magnetic field amplification in supernova remnants
• Magnetic fields in the formation of the first stars.--II Results
• A multi-shock model for the density variance of anisotropic, highly-magnetised, supersonic turbulence
• On the small scale turbulent dynamo in the intracluster medium: A comparison to dynamo theory
• Nonlinear turbulent dynamo during gravitational collapse
• Turbulence-induced magnetic fields in shock precursors
• Nonuniversal interstellar density spectra probed by pulsars
• Measuring magnetization with rotation measures and velocity centroids in supersonic MHD turbulence
• Shock acceleration with oblique and turbulent magnetic fields
• Study Turbulence and Probe Magnetic Field Using Gradients Technique: Application to HI-to-H2 Transition Regions
• Velocity Gradients: Magnetic Field Tomography towards the Supernova Remnant W44
• Discovery of Kolmogorov-like Magnetic Energy Spectrum in Tycho's Supernova Remnant by Two-point Correlations of Synchrotron Intensity
• Vortical amplification of magnetic field at inward shock of supernova remnant Cassiopeia A
• Particle acceleration in interstellar shocks

Cited by in corpus (12)

• Faraday Rotation Measure Variations of Repeating Fast Radio Burst Sources
• Turbulent reconnection acceleration
• Lagrangian statistics of a shock-driven turbulent dynamo in decaying turbulence
• X-ray polarization: A view deep inside cosmic ray driven turbulence and particle acceleration in supernova remnants
• Anisotropies of Diffusive Ultra-high Energy Cosmic Rays in $f(R)$ Gravity Theory
• Particle acceleration and magnetic field amplification by relativistic shocks in inhomogeneous media
• Magnetic Suppression of Cosmic Rays' Flux in $\mathbf{f}(\mathbf{R})$ and $\mathbf{f}(\mathbf{Q})$ Theories of Gravity
• PeV particle acceleration and non-thermal emission in the `minimalist' model of the extended jets in W50/SS433
• Analysing Ultra High Energy Cosmic Rays' Anisotropy in $\mathbf{f}(\mathbf{R},\mathbf{T})$ Gravity Theory
• Property of downstream turbulence driven by the special relativistic shock-clump interaction
• Modelling Cosmic Rays Flux with Pierre Auger and Telescope Array Data in $\mathbf{f}(\mathbf{R})$ and $\mathbf{f}(\mathbf{Q})$ Theories of Gravity
• Ultra-high energy cosmic rays with UFA-15 source model in Bumblebee gravity theory