Shock acceleration with oblique and turbulent magnetic fields
arXiv:2111.04759 · doi:10.3847/1538-4357/ac3824
Abstract
We investigate shock acceleration in a realistic astrophysical environment with density inhomogeneities. The turbulence induced by the interaction of the shock precursor with upstream density fluctuations amplifies both upstream and downstream magnetic fields via the turbulent dynamo. The dynamo-amplified turbulent magnetic fields (a) introduce variations of shock obliquities along the shock face, (b) enable energy gain through a combination of shock drift and diffusive processes, (c) give rise to various spectral indices of accelerated particles, (d) regulate the diffusion of particles both parallel and perpendicular to the magnetic field, and (e) increase the shock acceleration efficiency. Our results demonstrate that upstream density inhomogeneities and dynamo amplification of magnetic fields play an important role in shock acceleration, and thus shock acceleration depends on the condition of the ambient interstellar environment. The implications on understanding radio spectra of supernova remnants are also discussed.
arXiv comment17 pages, 12 figures, accepted for publication in ApJ
References in corpus (41)
- Reconnection in a Weakly Stochastic Field
- Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
- Simulations of Ion Acceleration at Non-relativistic Shocks. I. Acceleration Efficiency
- Compressible Turbulence in Galaxy Clusters: Physics and Stochastic Particle Re-acceleration
- Turbulent molecular clouds
- Scattering of Cosmic Rays by Magnetohydrodynamic Interstellar Turbulence
- The 1st Fermi Lat Supernova Remnant Catalog
- Extending Big Power Law in the Sky with Turbulence Spectra from WHAM data
- Simulations of Ion Acceleration at Non-relativistic Shocks. II. Magnetic Field Amplification
- Scattering of energetic particles by anisotropic magnetohydrodynamic turbulence with a Goldreich-Sridhar power spectrum
- Turbulence and Magnetic Field Amplification in Supernova Remnants: Interactions Between A Strong Shock Wave and Multi-Phase Interstellar Medium
- Enhancement and suppression of heat transfer by MHD turbulence
- Velocity Modification of Power Spectrum from Absorbing Medium
- Turbulence-induced magnetic fields and the structure of Cosmic Ray modified shocks
- Superdiffusion of Cosmic Rays: Implications for Cosmic Ray Acceleration
- Obtaining Spectra of Turbulent Velocity from Observations
- Cosmic Ray Parallel and Perpendicular Transport in Turbulent Magnetic Fields
- Cosmic ray acceleration at oblique shocks
- Turbulent dynamo in a conducting fluid and partially ionized gas
- The gas density around SN 1006
- Diffusion of cosmic rays in MHD turbulence with magnetic mirrors
- Turbulent magnetic field amplification driven by cosmic-ray pressure gradients
- On magnetic field amplification and particle acceleration near non-relativistic astrophysical shocks: Particles in MHD Cells simulations
- Magnetohydrodynamic-Particle-in-Cell Simulations of the Cosmic-Ray Streaming Instability: Linear Growth and Quasi-linear Evolution
- Scatter broadening of pulsars and implications on the interstellar medium turbulence
- Interpretation of the structure function of rotation measure in the interstellar medium
- On the radio spectra of supernova remnants
- Resonance-broadened transit time damping of particles in MHD turbulence
- The Efficiency of Magnetic Field Amplification at Shocks by Turbulence
- Trapping of cosmic rays in MHD turbulence
- Magnetic field amplification in supernova remnants
- On the supernova remnants with flat radio spectra
- Turbulence-induced magnetic fields in shock precursors
- Nonuniversal interstellar density spectra probed by pulsars
- Discovery of Kolmogorov-like Magnetic Energy Spectrum in Tycho's Supernova Remnant by Two-point Correlations of Synchrotron Intensity
- Mirror diffusion of cosmic rays in highly compressible turbulence near supernova remnants
- Effect of acceleration and escape of energetic particles on spectral steepening at shocks
- Steepening of Cosmic Ray Spectra in Shocks with Varying Magnetic Field Direction
- Turbulent dynamo in a weakly ionized medium
- Simulating TeV gamma-ray morphologies of shell-type supernova remnants
- Particle acceleration in interstellar shocks
Cited by in corpus (8)
- Massive star cluster origin for the galactic cosmic ray population at very-high energies
- Superdiffusion of Cosmic Rays in Compressible Magnetized Turbulence
- Turbulent Magnetic Field Amplification by the Interaction of Shock Wave and Inhomogeneous Medium
- Cosmic ray streaming in the turbulent interstellar medium
- Turbulent reconnection acceleration
- Quasi-perpendicular shock acceleration and TDE radio flares
- Modeling Hadronic Gamma-ray Emissions from Solar Flares and Prospects for Detecting Non-thermal Signatures from Protostars
- TeV-PeV Gamma-ray and Neutrino Emission in the Galactic Plane