Production of Magnetic Turbulence by Cosmic Rays Drifting Upstream of Supernova Remnant Shocks

Abstract

We present results of 2D and 3D PIC simulations of magnetic turbulence production by isotropic cosmic-ray ions drifting upstream of SNR shocks. The studies aim at testing recent predictions of a strong amplification of short wavelength magnetic field and at studying the evolution of the magnetic turbulence and its backreaction on cosmic rays. We observe that an oblique filamentary mode grows more rapidly than the non-resonant parallel modes found in analytical theory, and the growth rate of the field perturbations is much slower than is estimated for the parallel plane-wave mode, possibly because in our simulations we cannot maintain omega << Omega_i, the ion gyrofrequency, to the degree required for the plane-wave mode to emerge. The evolved oblique filamentary mode was also observed in MHD simulations to dominate in the nonlinear phase. We thus confirm the generation of the turbulent magnetic field due to the drift of cosmic-ray ions in the upstream plasma, but as our main result find that the amplitude of the turbulence saturates at about dB/B~1. The backreaction of the turbulence on the particles leads to an alignment of the bulk-flow velocities of the cosmic rays and the background medium, which is an essential characteristic of cosmic-ray modified shocks. It accounts for the saturation of the instability at moderate field amplitudes. Previously published MHD simulations have assumed a constant cosmic-ray current and no energy or momentum flux in the cosmic rays, which excludes a backreaction of the generated magnetic field on cosmic rays, and thus the saturation of the field amplitude is artificially suppressed. This may explain the continued growth of the magnetic field in the MHD simulations. A strong magnetic field amplification to amplitudes dB >> B0 has not been demonstrated yet.

revised version; accepted to ApJ; 36 pages, 13 figures

References in corpus (9)

• Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification
• Modeling Bell's Non-resonant Cosmic Ray Instability
• The transport of cosmic rays in self-excited magnetic turbulence
• A cosmic ray current driven instability in partially ionised media
• Turbulence and particle acceleration in collisionless supernovae remnant shocks: I-Anisotropic spectra solutions
• A current driven instability in parallel, relativistic shocks
• Turbulence and particle acceleration in collisionless supernovae remnant shocks: II- Cosmic-ray transport
• Magnetic Field Amplification and Rapid Time Variations in SNR RX J1713.7-3946
• Environmental limits on the non-resonant cosmic-ray current-driven instability

Cited by in corpus (39)

• A kinetic approach to cosmic ray induced streaming instability at supernova shocks
• The origin of galactic cosmic rays
• Turbulence Dissipation and Particle Injection in Non-Linear Diffusive Shock Acceleration with Magnetic Field Amplification
• On Fermi acceleration and MHD-instabilities at ultra-relativistic magnetized shock waves
• The Heating of Thermal Electrons in Fast Collisionless Shocks: The Integral Role of Cosmic Rays
• PIC methods in astrophysics: Simulations of relativistic jets and kinetic physics in astrophysical systems
• X-ray Stripes in Tycho's Supernova Remant: Synchrotron Footprints of a Nonlinear Cosmic Ray-driven Instability
• Magnetic field amplification by the Weibel instability at planetary and astrophysical high-Mach-number shocks
• PIC Simulation Methods for Cosmic Radiation and Plasma Instabilities
• Electron Pre-Acceleration at Nonrelativistic High-Mach-Number Perpendicular Shocks
• Kinetic simulations of nonrelativistic perpendicular shocks of young supernova remnants. III. Magnetic reconnection
• Kinetic simulations of nonrelativistic perpendicular shocks of young supernova remnants. I. Electron shock-surfing acceleration
• Reacceleration of electrons in supernova remnants
• Electron Acceleration at Rippled Low-Mach-number Shocks in High-beta Collisionless Cosmic Plasmas
• Kinetic simulation of nonrelativistic perpendicular shocks of young supernova remnants. IV. Electron heating
• Lepton-driven Non-resonant Streaming Instability
• Mildly relativistic magnetized shocks in electron-ion plasmas -- II. Particle acceleration and heating
• Pre-acceleration in the Electron Foreshock I: Electron Acoustic Waves
• Spatio-temporal evolution of the nonresonant instability in shock precursors of young supernova remnants
• Fast Particle Acceleration at Perpendicular Shocks with Uniform Upstream Magnetic Field and Strong Downstream Turbulence
• The Biermann battery driven by a streaming plasma
• Mildly relativistic magnetized shocks in electron-ion plasmas I. Electromagnetic shock structure
• Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields
• Diffusive shock acceleration at oblique high Mach number shocks
• Self-discharge by streaming cosmic rays
• Particle acceleration, escape and non-thermal emission from core-collapse supernovae inside non-identical wind-blown bubbles
• Nonthermal properties of supernova remnant G1.9+0.3
• 3D PIC Simulations for Relativistic Jets with a Toroidal Magnetic Field
• Particle acceleration in a shock wave propagating to an inhomogeneous medium
• Resistive Heating Induced by Streaming Cosmic Rays Around a Galaxy in the Early Universe
• How to turn a Supernova into a PeVatron
• Escape of cosmic rays from perpendicular shocks in the circumstellar magnetic field
• Modeling Magnetic Field Amplification in Nonlinear Diffusive Shock Acceleration
• Macroscopic magnetization of primordial plasma by virial shocks
• From electrons to Janskys: Full stokes polarized radiative transfer in 3D relativistic particle-in-cell jet simulations
• The electron foreshock at high-Mach-number nonrelativistic oblique shocks
• Escape of cosmic rays from perpendicular shocks in the interstellar magnetic field
• Non-resonant Streaming Instability driven by Leptons
• Time-dependent treatment of cosmic-ray spectral steepening due to turbulence driving