arXiv subjects

Guy Pelletier

Publications and source records attributed to Guy Pelletier.

21 records · Page 2Linked to original sources

arXiv2001

Transport of Cosmic Rays in Chaotic Magnetic Fields

The transport of charged particles in disorganised magnetic fields is an important issue which concerns the propagation of cosmic rays of all energies in a variety of astrophysical environments, such as the interplanetary, interstellar and even extra-galactic media, as well as the efficiency of Fermi acceleration processes. We have performed detailed numerical experiments using Monte-Carlo simulations of particle propagation in stochastic magnetic fields in order to measure the parallel and transverse spatial diffusion coefficients and the pitch angle scattering time as a function of rigidity and strength of the turbulent magnetic component. We confirm the extrapolation to high turbulence levels of the scaling predicted by the quasi-linear approximation for the scattering frequency and parallel diffusion coefficient at low rigidity. We show that the widely used Bohm diffusion coefficient does not provide a satisfactory approximation to diffusion even in the extreme case where the mean field vanishes. We find that diffusion also takes place for particles with Larmor radii larger than the coherence length of the turbulence. We argue that transverse diffusion is much more effective than predicted by the quasi-linear approximation, and appears compatible with chaotic magnetic diffusion of the field lines. We provide numerical estimates of the Kolmogorov length and magnetic line diffusion coefficient as a function of the level of turbulence. Finally we comment on applications of our results to astrophysical turbulence and the acceleration of high energy cosmic rays in supernovae remnants, in super-bubbles, and in jets and hot spots of powerful radio-galaxies.

astro-ph↗

arXiv2000

Pressure- and magnetic shear- driven instabilities in rotating MHD jets

We derive new stability criteria for purely MHD instabilities in rotating jets, in the framework of the ballooning ordering expansion. Quite unexpectedly, they involve a term which is linear in the magnetic shear. This implies that cylindrical configurations can be destabilized by a negative magnetic shear as well as by a favorable equilibrium pressure gradient, in distinction with the predictions of Suydam's stability criterion, which suggests on the contrary that the shear is always stabilizing. We have used these criteria to establish sufficient conditions for instability. In particular, the magnetic shear can always destabilize jets with vanishing current density on the axis, a feature which is generically found in jets which are launched from an accretion disk. We also show that standard nonrotating jet models (where the toroidal field dominates the poloidal one), which are known to be unstable, are not stabilized by rotation, unless the plasma $β$ parameter and the strength of the rotation forces are both close to the limit allowed by the condition of radial equilibrium. The new magnetic shear-driven instability found in this paper, as well as the more conventional pressure-driven instability, might provide us with a potential energy source for the particle acceleration mechanisms underlying the high energy emission which takes place in the interior of AGN jets.

astro-ph↗

arXiv2000

Acceleration of UHE Cosmic Rays in Gamma-Ray Bursts

Gamma-Ray Bursts are good candidates of the ``bottom up'' scenario for the generation of the UHE Cosmic Rays. In the most discussed model of GRBs, namely the ``fireball'' model, a highly relativistic shock forms and seems capable of accelerating the cosmic rays up to the EeV range. However, only the first Fermi cycle produces a large energy gain to particles coming from the external medium. Thus, a complementary acceleration is proposed, downstream of the external shock, in the relativistic plasma of the GRBs, where crossings of relativistic fronts are likely to occur. Both forward and backward fronts are necessary for the internal Fermi acceleration to work and the physical process that generates them is presented. We found that there exists a relevant physical process similar to Brillouin backscattering that redistributes the incoming energy in the plasma shell. This redistribution occurs through the generation of sound waves that heat the plasma shell and also through the generation of both forward and backward relativistic Alfven fronts that accelerate cosmic rays by the Fermi process. We show that this ensemble of processes is able to account for the generation of UHE cosmic rays. There are two opportunities for these combined processes, first during the ``primary'' Gamma-Ray Burst where baryons are entrained by the relativistic pair wind, second during the predeceleration and deceleration stages when the fireball interacts with the interstellar medium. However, because of the synchrotron losses, only the second stage can produce the UHE cosmic rays.

astro-ph↗