Turbulence and particle acceleration in collisionless supernovae remnant shocks. II. Cosmic-ray transport

@article{Marcowith2006TurbulenceAP,
  title={Turbulence and particle acceleration in collisionless supernovae remnant shocks. II. Cosmic-ray transport},
  author={Alexandre Marcowith and Martin Lemoine and Guy Pelletier},
  journal={Astronomy and Astrophysics},
  year={2006},
  volume={453},
  pages={193-202}
}
Supernovae remnant shock waves could be at the origin of cosmic rays up to energies in excess of the knee ($E\simeq3\times 10^{15}\,$eV) if the magnetic field is efficiently amplified by the streaming of accelerated particles in the shock precursor. This paper follows up on a previous paper (Pelletier et al. 2006, A&A, in press) which derived the properties of the MHD turbulence so generated, in particular its anisotropic character, its amplitude and its spectrum. In the present paper, we… 

Figures from this paper

Turbulence and particle acceleration in collisionless supernovae remnant shocks. I. Anisotropic spec
This paper investigates the nature of the MHD turbulence excited by the streaming of accelerated cosmic rays in a shock wave precursor. The two recognised regimes (non-resonant and resonant) of the
Production of Magnetic Turbulence by Cosmic Rays Drifting Upstream of Supernova Remnant Shocks
We present results of two- and three-dimensional particle-in-cell simulations of magnetic turbulence production by isotropic cosmic-ray ions drifting upstream of supernova remnant shocks. The studies
Cosmic Ray propagation in sub-Alfvenic magnetohydrodynamic turbulence
This work has the main objective to provide a detailed investigation of cosmic ray propagation in magnetohydrodynamic turbulent fields generated by forcing the fluid velocity field at large scales.
Core-collapse supernovae as cosmic ray sources.
TLDR
This study calculates the growth time-scales of CR-driven instabilities and finds that extended IIb SNe shocks can trigger fast intra-day instabilities, strong magnetic field amplification, and CR acceleration, and the trans-relativistic object SN 2009bb can accelerate CRs up to 2-3 PeV within 20 d after the outburst.
KINETIC SIMULATIONS OF TURBULENT MAGNETIC-FIELD GROWTH BY STREAMING COSMIC RAYS
Efficient acceleration of cosmic rays (via the mechanism of diffusive shock acceleration) requires turbulent, amplified magnetic fields in the shock's upstream region. We present results of
Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J
Aims. The extensive observations of the supernova SN 1993J at radio wavelengths make this object a unique target for the study of particle acceleration in a supernova shock. Methods. To describe the
Particle spectra and efficiency in nonlinear relativistic shock acceleration - survey of scattering models
We include a general form for the scattering mean free path in a nonlinear Monte Carlo model of relativistic shock formation and Fermi acceleration. Particle-in-cell (PIC) simulations, as well as
The microphysics of collisionless shock waves.
TLDR
This review adresses the physics of shock formation, shock dynamics and particle acceleration based on a close examination of available multi-wavelength or in situ observations, analytical and numerical developments and focuses on the different instabilities triggered during the shock formation and in association with particle acceleration processes.
Postshock turbulence and diffusive shock acceleration in young supernova remnants
Thin X-ray filaments are observed in the vicinity of young supernova remnants (SNR) blast waves. Identifying processes involved in the creation of such filaments would provide a direct insight of
Magnetic Fields in Cosmic Particle Acceleration Sources
We review here some magnetic phenomena in astrophysical particle accelerators associated with collisionless shocks in supernova remnants, radio galaxies and clusters of galaxies. A specific feature
...
...

References

SHOWING 1-10 OF 50 REFERENCES
Turbulence and particle acceleration in collisionless supernovae remnant shocks. I. Anisotropic spec
This paper investigates the nature of the MHD turbulence excited by the streaming of accelerated cosmic rays in a shock wave precursor. The two recognised regimes (non-resonant and resonant) of the
Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation
The instability in the cosmic-ray precursor of a supernova shock moving in interstellar medium is studied. The level of magnetohydrodynamic turbulence in this region determines the maximum energy of
Hydrodynamic simulation of supernova remnants including efficient particle acceleration
A number of supernova remnants (SNRs) show nonthermal X-rays assumed to be synchrotron emission from shock accelerated TeV electrons. The existence of these TeV electrons strongly suggests that the
On the spectrum of high-energy cosmic rays produced by supernova remnants in the presence of strong cosmic-ray streaming instability and wave dissipation
The cosmic-ray streaming instability creates strong magnetohydrodynamic turbulence in the precursor of a SN shock. The level of turbulence determines the maximum energy of cosmic-ray particles
Shocks and particle acceleration in SNRs: theoretical aspects
Direct evidence of efficient cosmic ray acceleration and magnetic field amplification in Cassiopeia A
It is shown that the nonlinear kinetic theory of cosmic ray (CR) acceleration in supernova remnants (SNRs) describes the shell-type nonthermal X-ray morphology of Cas A, obtained in Chandra
The Anisotropy of MHD Alfv\'{e}nic Turbulence
We perform direct 3-dimensional numerical simulations for magnetohydrodynamic (MHD) turbulence in a periodic box of size $2\pi$ threaded by strong uniform magnetic fields. We use a pseudo-spectral
Can diffusive shock acceleration in supernova remnants account for high-energy galactic cosmic rays?
Diffusive shock acceleration at the outer front of expanding supernova remnants has provided by far the most popular model for the origin of galactic cosmic rays, and has been the subject of
Time-dependent Simulation of Cosmic-Ray Shocks, Including Alfven Transport
Time evolution of plane, cosmic-ray modified shocks has been simulated numerically for the case with parallel magnetic fields. Computations were done in a 'three-fluid' dynamical model incorporating
...
...