39 research outputs found
In-situ Particle Acceleration in Collisionless Shocks
The outflows from gamma ray bursts, active galactic nuclei and relativistic
jets in general interact with the surrounding media through collisionless
shocks. With three dimensional relativistic particle-in-cell simulations we
investigate such shocks. The results from these experiments show that
small--scale magnetic filaments with strengths of up to percents of
equipartition are generated and that electrons are accelerated to power law
distributions N(E)~E^{-p} in the vicinity of the filaments through a new
acceleration mechanism. The acceleration is locally confined, instantaneous and
differs from recursive acceleration processes such as Fermi acceleration. We
find that the proposed acceleration mechanism competes with thermalization and
becomes important at high Lorentz factors.Comment: 4 pages, 2 figures, submitted to Il nuovo cimento (4th Workshop
Gamma-Ray Bursts in the Afterglow Era, Rome, 18-22 October 2004
Non-Fermi Power law Acceleration in Astrophysical Plasma Shocks
Collisionless plasma shock theory, which applies for example to the afterglow
of gamma ray bursts, still contains key issues that are poorly understood. In
this paper we study charged particle dynamics in a highly relativistic
collisionless shock numerically using ~10^9 particles. We find a power law
distribution of accelerated electrons, which upon detailed investigation turns
out to originate from an acceleration mechanism that is decidedly different
from Fermi acceleration.
Electrons are accelerated by strong filamentation instabilities in the
shocked interpenetrating plasmas and coincide spatially with the power law
distributed current filamentary structures. These structures are an inevitable
consequence of the now well established Weibel-like two-stream instability that
operates in relativistic collisionless shocks.
The electrons are accelerated and decelerated instantaneously and locally; a
scenery that differs qualitatively from recursive acceleration mechanisms such
as Fermi acceleration.
The slopes of the electron distribution power laws are in concordance with
the particle power law spectra inferred from observed afterglow synchrotron
radiation in gamma ray bursts, and the mechanism can possibly explain more
generally the origin of non-thermal radiation from shocked inter- and
circum-stellar regions and from relativistic jets.Comment: 4 pages accepted for publication in ApJ Letters. High resolution
figures are available online at http://www.astro.ku.dk/users/hededal/040855
Acceleration Mechanics in Relativistic Shocks by the Weibel Instability
Plasma instabilities (e.g., Buneman, Weibel and other two-stream
instabilities) created in collisionless shocks may be responsible for particle
(electron, positron, and ion) acceleration. Using a 3-D relativistic
electromagnetic particle (REMP) code, we have investigated long-term particle
acceleration associated with relativistic electron-ion or electron-positron jet
fronts propagating into an unmagnetized ambient electron-ion or
electron-positron plasma. These simulations have been performed with a longer
simulation system than our previous simulations in order to investigate the
nonlinear stage of the Weibel instability and its particle acceleration
mechanism. The current channels generated by the Weibel instability are
surrounded by toroidal magnetic fields and radial electric fields. This radial
electric field is quasi stationary and accelerates particles which are then
deflected by the magnetic field.Comment: 17 pages, 5 figures, accepted for publication in ApJ, A full
resolution ot the paper can be found at
http://gammaray.nsstc.nasa.gov/~nishikawa/accmec.pd
Particle Acceleration, Magnetic Field Generation, and Associated Emission in Collisionless Relativistic Jets
Nonthermal radiation observed from astrophysical systems containing
relativistic jets and shocks, e.g., active galactic nuclei (AGNs), gamma-ray
bursts (GRBs), and Galactic microquasar systems usually have power-law emission
spectra. Recent PIC simulations using injected relativistic electron-ion
(electro-positron) jets show that acceleration occurs within the downstream
jet. Shock acceleration is a ubiquitous phenomenon in astrophysical plasmas.
Plasma waves and their associated instabilities (e.g., the Buneman instability,
other two-streaming instability, and the Weibel instability) created in the
shocks are responsible for particle (electron, positron, and ion) acceleration.
The simulation results show that the Weibel instability is responsible for
generating and amplifying highly nonuniform, small-scale magnetic fields. These
magnetic fields contribute to the electron's transverse deflection behind the
jet head. The ``jitter'' radiation from deflected electrons has different
properties than synchrotron radiation which assumes a uniform magnetic field.
This jitter radiation may be important to understanding the complex time
evolution and/or spectral structure in gamma-ray bursts, relativistic jets, and
supernova remnants.Comment: 4 pages, 3 figures, contributed talk at the workshop: High Energy
Phenomena in Relativistic Outflows (HEPRO), Dublin, 24-28 September 2007.
Fig. 3 is replaced by the correct versio
Particle acceleration, magnetic field generation, and emission in relativistic pair jets
Shock acceleration is a ubiquitous phenomenon in astrophysical plasmas.
Plasma waves and their associated instabilities (e.g., Buneman, Weibel and
other two-stream instabilities) created in collisionless shocks are responsible
for particle (electron, positron, and ion) acceleration. Using a 3-D
relativistic electromagnetic particle (REMP) code, we have investigated
particle acceleration associated with a relativistic jet front propagating into
an ambient plasma. We find that the growth times of Weibel instability are
proportional to the Lorentz factors of jets. Simulations show that the Weibel
instability created in the collisionless shock front accelerates jet and
ambient particles both perpendicular and parallel to the jet propagation
direction.Comment: 4 pages, 2 figures, submitted to Il nuovo cimento (4th Workshop
Gamma-Ray Bursts in the Afterglow Era, Rome, 18-22 October 2004
Magnetic Field Generation in Collisionless Shocks; Pattern Growth and Transport
We present results from three-dimensional particle simulations of
collisionless shocks with relativistic counter-streaming ion-electron plasmas.
Particles are followed over many skin depths downstream of the shock. Open
boundaries allow the experiments to be continued for several particle crossing
times. The experiments confirm the generation of strong magnetic and electric
fields by a Weibel-like kinetic streaming instability, and demonstrate that the
electromagnetic fields propagate far downstream of the shock. The magnetic
fields are predominantly transversal, and are associated with merging ion
current channels. The total magnetic energy grows as the ion channels merge,
and as the magnetic field patterns propagate down stream. The electron
populations are quickly thermalized, while the ion populations retain distinct
bulk speeds in shielded ion channels and thermalize much more slowly. These
results may help explain the origin of the magnetic fields responsible for
afterglow synchrotron/jitter radiation from Gamma-Ray Bursts.Comment: 4 pages, 6 figures - Accepted to ApJL. Revised version following
recommendations of referee report. Content reduced marginally. Conclusions
unchange
Particle acceleration in electron-ion jets
Weibel instability created in collisionless shocks is responsible for
particle (electron, positron, and ion) acceleration. Using a 3-D relativistic
electromagnetic particle (REMP) code, we have investigated particle
acceleration associated with a relativistic electron-ion jet fronts propagating
into an ambient plasma without initial magnetic fields with a longer simulation
system in order to investigate nonlinear stage of the Weibel instability and
its acceleration mechanism. The current channels generated by the Weibel
instability induce the radial electric fields. The z component of the Poynting
vector (E x B) become positive in the large region along the jet propagation
direction. This leads to the acceleration of jet electrons along the jet. In
particular the E x B drift with the large scale current channel generated by
the ion Weibel instability accelerate electrons effectively in both parallel
and perpendicular directions.Comment: 2 pages, 1 figure, Proceedings for Astrophysical Sources of High
Energy Particles and Radiation, AIP proceeding Series, eds . T. Bulik, G.
Madejski and B. Ruda
Relativistic Shocks: Particle Acceleration and Magnetic Field Generation, and Emission
Shock acceleration is an ubiquitous phenomenon in astrophysical plasmas.
Plasma waves and their associated instabilities (e.g.,Buneman, Weibel and other
two-stream instabilities) created in collisionless shocks are responsible for
particle (electron, positron, and ion) acceleration. Using a 3-D relativistic
electromagnetic particle (REMP) code, we have investigated particle
acceleration associated with a relativistic jet front propagating into an
ambient plasma with and without initial magnetic fields. Simulations show that
the Weibel instability created in the collisionless shock front accelerates jet
and ambient particles both perpendicular and parallel to the jet propagation
direction. The non-linear fluctuation amplitudes of densities, currents,
electric, and magnetic fields in the electron-positron shock are larger than
those found in the electron-ion shock at the same simulation time. This comes
from the fact that both electrons and positrons contribute to generation of the
Weibel instability. The simulation results show that the Weibel instability is
responsible for generating and amplifying nonuniform, small-scale (mainly
transverse) magnetic fields which contribute to the electron's (positron's)
transverse deflection behind the jet head. This small scale magnetic field
structure is appropriate to the generation of ``jitter'' radiation from
deflected electrons (positrons) as opposed to synchrotron radiation.Comment: 6 pages, 2 figures, submitted to Proceeding of International
Symposium on High Energy Gamma-Ray Astronomy (July 26-30, 2004