Diffusive shock re-acceleration

@article{Caprioli2018DiffusiveSR,
  title={Diffusive shock re-acceleration},
  author={Damiano Caprioli and Horace Zhang and Anatoly Spitkovsky},
  journal={Journal of Plasma Physics},
  year={2018},
  volume={84}
}
We have performed two-dimensional hybrid simulations of non-relativistic collisionless shocks in the presence of pre-existing energetic particles (‘seeds’); such a study applies, for instance, to the re-acceleration of galactic cosmic rays (CRs) in supernova remnant (SNR) shocks and solar wind energetic particles in heliospheric shocks. Energetic particles can be effectively reflected and accelerated regardless of shock inclination via a process that we call diffusive shock re-acceleration. We… 

Kinetic Simulations of Cosmic-Ray-modified Shocks. I. Hydrodynamics

Collisionless plasma shocks are efficient sources of nonthermal particle acceleration in space and astrophysical systems. We use hybrid (kinetic ion—fluid electron) simulations to examine the

Particle acceleration and non-thermal emission in colliding-wind binary systems

We present a model for the creation of non-thermal particles via diffusive shock acceleration in a colliding-wind binary. Our model accounts for the oblique nature of the global shocks bounding the

Shock-accelerated cosmic rays and streaming instability in the adaptive mesh refinement code Ramses

Cosmic rays (CRs) are thought to play a dynamically important role in several key aspects of galaxy evolution, including the structure of the interstellar medium, the formation of galactic winds, and

Diffusive acceleration in relativistic shocks: particle feedback

The spectral index s of high-energy particles diffusively accelerated in a non-magnetized relativistic shock, such as in a γ-ray burst afterglow, depends on the unknown angular diffusion function

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.

Gamma-rays from reaccelerated particles at supernova remnant shocks

Diffusive shock acceleration is considered as the main mechanism for particle energization in supernova remnants, as well as in other classes of sources. The existence of some remnants that show a

Electron Acceleration in One-dimensional Nonrelativistic Quasi-perpendicular Collisionless Shocks

We study diffusive shock acceleration (DSA) of electrons in nonrelativistic quasi-perpendicular shocks using self-consistent one-dimensional particle-in-cell simulations. By exploring the parameter

Acceleration of cosmic rays by double shock waves in galaxy clusters: application to radio relics

Context. Radio relics in galaxy clusters are known to be good laboratories for verification of the applicability of the diffusive shock acceleration (DSA) model in its canonical version. The need for

dHybridR: A Hybrid Particle-in-cell Code Including Relativistic Ion Dynamics

We present the first plasma simulations obtained with the code dHybridR, a hybrid particle-in-cell code with fluid electrons and both thermal and energetic ions that retain relativistic dynamics.

Turbulence and Energetic Particles in Radiative Shock Waves in the Cygnus Loop. I. Shock Properties

We have obtained a contiguous set of long-slit spectra of a shock wave in the Cygnus Loop to investigate its structure, which is far from the morphology predicted by 1D models. Proper motions from

References

SHOWING 1-10 OF 77 REFERENCES

COSMIC-RAY-INDUCED FILAMENTATION INSTABILITY IN COLLISIONLESS SHOCKS

We used unprecedentedly large two-dimensional and three-dimensional hybrid (kinetic ions—fluid electrons) simulations of non-relativistic collisionless strong shocks in order to investigate the

SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. III. PARTICLE DIFFUSION

We use large hybrid (kinetic-protons–fluid-electrons) simulations to investigate the transport of energetic particles in self-consistent electromagnetic configurations of collisionless shocks. In

Simulations and Theory of Ion Injection at Non-relativistic Collisionless Shocks

We use kinetic hybrid simulations (kinetic ions–fluid electrons) to characterize the fraction of ions that are accelerated to non-thermal energies at non-relativistic collisionless shocks. We

Simulating cosmic ray physics on a moving mesh

We discuss new methods to integrate the cosmic ray (CR) evolution equations coupled to magneto-hydrodynamics (MHD) on an unstructured moving mesh, as realised in the massively parallel AREPO code for

Ion acceleration in non-relativistic astrophysical shocks

We explore the physics of shock evolution and particle acceleration in non-relativistic collisionless shocks using hybrid simulations. We analyze a wide range of physical parameters relevant to the

Simulations of Ion Acceleration at Non-relativistic Shocks. I. Acceleration Efficiency

We use two-dimensional and three-dimensional hybrid (kinetic ions–fluid electrons) simulations to investigate particle acceleration and magnetic field amplification at non-relativistic astrophysical

PARTICLE ACCELERATION IN RELATIVISTIC MAGNETIZED COLLISIONLESS ELECTRON-ION SHOCKS

We investigate shock structure and particle acceleration in relativistic magnetized collisionless electron–ion shocks by means of 2.5-dimensional particle-in-cell simulations with ion-to-electron

MAGNETIC AMPLIFICATION BY MAGNETIZED COSMIC RAYS IN SUPERNOVA REMNANT SHOCKS

X-ray observations of synchrotron rims in supernova remnant (SNR) shocks show evidence of efficient electron acceleration and strong magnetic field amplification (a factor of ∼100 between the

PARTICLE ACCELERATION IN RELATIVISTIC MAGNETIZED COLLISIONLESS PAIR SHOCKS: DEPENDENCE OF SHOCK ACCELERATION ON MAGNETIC OBLIQUITY

We investigate shock structure and particle acceleration in relativistic magnetized collisionless pair shocks by means of 2.5D and 3D particle-in-cell simulations. We explore a range of inclination

Universal behaviour of shock precursors in the presence of efficient cosmic ray acceleration

The self-consistent interaction between energetic particles and self-generated hydromagnetic waves in a cosmic-ray pressure dominated plasma is considered. Using a three-dimensional hybrid
...