709 research outputs found
Multidimensional simulations of magnetic field amplification and electron acceleration to near-energy equipartition with ions by a mildly relativistic quasi-parallel plasma collision
The energetic electromagnetic eruptions observed during the prompt phase of
gamma-ray bursts are attributed to synchrotron emissions. The internal shocks
moving through the ultrarelativistic jet, which is ejected by an imploding
supermassive star, are the likely source of this radiation. Synchrotron
emissions at the observed strength require the simultaneous presence of
powerful magnetic fields and highly relativistic electrons. We explore with one
and three-dimensional relativistic particle-in-cell simulations the transition
layer of a shock, that evolves out of the collision of two plasma clouds at a
speed 0.9c and in the presence of a quasi-parallel magnetic field. The cloud
densities vary by a factor of 10. The number densities of ions and electrons in
each cloud, which have the mass ratio 250, are equal. The peak Lorentz factor
of the electrons is determined in the 1D simulation, as well as the orientation
and the strength of the magnetic field at the boundary of the two colliding
clouds. The relativistic masses of the electrons and ions close to the shock
transition layer are comparable as in previous work. The 3D simulation shows
rapid and strong plasma filamentation behind the transient precursor. The
magnetic field component orthogonal to the initial field direction is amplified
in both simulations to values that exceed those expected from the shock
compression by over an order of magnitude. The forming shock is
quasi-perpendicular due to this amplification. The simultaneous presence of
highly relativistic electrons and strong magnetic fields will give rise to
significant synchrotron emissions.Comment: 8 pages, 5 figures. This work was presented at 21st International
Conference on Numerical Simulation of Plasmas (ICNSP'09). Accepted for
publication IEEE Trans. on Plasma Scienc
The influence of the mass-ratio on the acceleration of particles by filamentation instabilities
Almost all sources of high energy particles and photons are associated with
jet phenomena. Prominent sources of such highly relativistic outflows are
pulsar winds and Active Galactic Nuclei. The current understanding of these
jets assumes diluted plasmas which are best described as kinetic phenomena. In
this kinetic description particle acceleration to ultra-relativistic speeds can
occur in completely unmagnetized and neutral plasmas through insetting effects
of instabilities. Even though the morphology and nature of particle spectra are
understood to a certain extent, the composition of the jets is not known yet.
While Poynting-flux dominated jets are certainly composed of electron-positron
plasmas, the understanding of the governing physics in AGN jets is mostly
unclear. In this article we investigate how the constituting elements of an
electron-positron-proton plasma behave differently under the variation of the
fundamental mass-ratio m_p/m_e. We studied initially unmagnetized
counterstreaming plasmas using fully relativistic three-dimensional
particle-in-cell simulations to investigate the influence of the mass-ratio on
particle acceleration and magnetic field generation in electron-positron-proton
plasmas. We covered a range of mass-ratios m_p/m_e between 1 and 100 with a
particle number composition of n_{p^+}/n_{e^+} of 1 in one stream, only protons
are injected in the other, whereas electrons are present in both to guarantee
charge neutrality in the simulation box. We find that with increasing proton
mass the instability takes longer to develop and for mass-ratios > 20 the
particles seem to be accelerated in two phases which can be accounted to the
individual instabilities of the different species. This means that for high
mass ratios the coupling between electrons/positrons and the heavier protons,
which occurs in low mass-ratios, disappears.Comment: 15 pages, 6 figure
Magnetic field amplification and electron acceleration to near-energy equipartition with ions by a mildly relativistic quasi-parallel plasma protoshock
The prompt emissions of gamma-ray bursts are seeded by radiating
ultrarelativistic electrons. Internal shocks propagating through a jet launched
by a stellar implosion, are expected to amplify the magnetic field & accelerate
electrons. We explore the effects of density asymmetry & a quasi-parallel
magnetic field on the collision of plasma clouds. A 2D relativistic PIC
simulation models the collision of two plasma clouds, in the presence of a
quasi-parallel magnetic field. The cloud density ratio is 10. The densities of
ions & electrons & the temperature of 131 keV are equal in each cloud. The mass
ratio is 250. The peak Lorentz factor of the electrons is determined, along
with the orientation & strength of the magnetic field at the cloud collision
boundary. The magnetic field component orthogonal to the initial plasma flow
direction is amplified to values that exceed those expected from shock
compression by over an order of magnitude. The forming shock is
quasi-perpendicular due to this amplification, caused by a current sheet which
develops in response to the differing deflection of the incoming upstream
electrons & ions. The electron deflection implies a charge separation of the
upstream electrons & ions; the resulting electric field drags the electrons
through the magnetic field, whereupon they acquire a relativistic mass
comparable to the ions. We demonstrate how a magnetic field structure
resembling the cross section of a flux tube grows in the current sheet of the
shock transition layer. Plasma filamentation develops, as well as signatures of
orthogonal magnetic field striping. Localized magnetic bubbles form. Energy
equipartition between the ion, electron & magnetic energy is obtained at the
shock transition layer. The electronic radiation can provide a seed photon
population that can be energized by secondary processes (e.g. inverse Compton).Comment: 12 pages, 15 Figures, accepted to A&
Two-stream-like instability in dilute hot relativistic beams and astrophysical relativistic shocks
Relativistic collisionless shocks are believed to be efficient particle
accelerators. Nonlinear outcome of the interaction of accelerated particles
that run ahead of the shock, the so-called "precursor", with the unperturbed
plasma of the shock upstream, is thought to facilitate additional acceleration
of these particles and to possibly modify the hydrodynamic structure of the
shock. We explore here the linear growth of kinetic modes appearing in the
precursor-upstream interaction in relativistic shocks propagating in non and
weakly magnetized plasmas: electrostatic two-stream parallel mode and
electrostatic oblique modes. These modes are of particular interest because
they are the fastest growing modes known in this type of system. Using a
simplified distribution function for a dilute ultra-relativistic beam that is
relativistically hot in its own rest frame, yet has momenta that are narrowly
collimated in the frame of the cold upstream plasma into which it propagates,
we identify the fastest growing mode in the full -space and calculate its
growth rate. We consider all types of plasma (pairs and ions-electrons) and
beam (charged and charge-neutral). We find that unstable electrostatic modes
are present in any type of plasma and for any shock parameters. We further find
that two modes, one parallel () and the other one oblique (), are competing for dominance and that either one may dominate the
growth rate in different regions of the phase space. The dominant mode is
determined mostly by the perpendicular spread of the accelerated particle
momenta in the upstream frame, which reflects the shock Lorentz factor. The
parallel mode becomes more dominant in shocks with lower Lorentz factors (i.e.,
with larger momentum spreads). We briefly discuss possible implications of our
results for external shocks in gamma-ray burst sources
Particle-in-cell simulation of a mildly relativistic collision of an electron-ion plasma carrying a quasi-parallel magnetic field: Electron acceleration and magnetic field amplification at supernova shocks
Plasma processes close to SNR shocks result in the amplification of magnetic
fields and in the acceleration of electrons, injecting them into the diffusive
acceleration mechanism. The acceleration of electrons and the B field
amplification by the collision of two plasma clouds, each consisting of
electrons and ions, at a speed of 0.5c is investigated. A quasi-parallel
guiding magnetic field, a cloud density ratio of 10 and a plasma temperature of
25 keV are considered. A quasi-planar shock forms at the front of the dense
plasma cloud. It is mediated by a circularly left-hand polarized
electromagnetic wave with an electric field component along the guiding
magnetic field. Its propagation direction is close to that of the guiding field
and orthogonal to the collision boundary. It has a low frequency and a
wavelength that equals several times the ion inertial length, which would be
indicative of a dispersive Alfven wave close to the ion cyclotron resonance
frequency of the left-handed mode (ion whistler), provided that the frequency
is appropriate. However, it moves with the super-alfvenic plasma collision
speed, suggesting that it is an Alfven precursor or a nonlinear MHD wave such
as a Short Large-Amplitude Magnetic Structure (SLAMS). The growth of the
magnetic amplitude of this wave to values well in excess of those of the
quasi-parallel guiding field and of the filamentation modes results in a
quasi-perpendicular shock. We present evidence for the instability of this mode
to a four wave interaction. The waves developing upstream of the dense cloud
give rise to electron acceleration ahead of the collision boundary. Energy
equipartition between the ions and the electrons is established at the shock
and the electrons are accelerated to relativistic speeds.Comment: 16 pages, 18 figures, Accepted for publication by Astron & Astrophy
Particle transport and heating in the microturbulent precursor of relativistic shocks
Collisionless relativistic shocks have been the focus of intense theoretical
and numerical investigations in recent years. The acceleration of particles,
the generation of electromagnetic microturbulence and the building up of a
shock front are three interrelated essential ingredients of a relativistic
collisionless shock wave. In this paper we investigate two issues of importance
in this context: (1) the transport of suprathermal particles in the excited
microturbulence upstream of the shock and its consequences regarding particle
acceleration; (2) the preheating of incoming background electrons as they cross
the shock precursor and experience relativistic oscillations in the
microturbulent electric fields. We place emphasis on the importance of the
motion of the electromagnetic disturbances relatively to the background plasma
and to the shock front. This investigation is carried out for the two major
instabilities involved in the precursor of relativistic shocks, the
filamentation instability and the oblique two stream instability. Finally, we
use our results to discuss the maximal acceleration at the external shock of a
gamma-ray burst; we find in particular a maximal synchrotron photon energy of
the order of a few GeV.Comment: 14 pages, 6 figures. Revised versio
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
Conditions for the onset of the current filamentation instability in the laboratory
Current Filamentation Instability (CFI) is capable of generating strong
magnetic fields relevant to explain radiation processes in astrophysical
objects and lead to the onset of particle acceleration in collisionless shocks.
Probing such extreme scenarios in the laboratory is still an open challenge. In
this work, we investigate the possibility of using neutral
beams to explore the CFI with realistic parameters, by performing 2D
particle-in-cell simulations. We show that CFI can occur unless the rate at
which the beam expands due to finite beam emittance is larger than the CFI
growth rate and as long as the role of competing electrostatic two-stream
instability (TSI) is negligible. We also show that the longitudinal energy
spread, typical of plasma based accelerated electron-positron fireball beams,
plays a minor role in the growth of CFI in these scenarios
Relativistic Particle-In-Cell Simulation Studies of Prompt and Early Afterglows from GRBs
Nonthermal radiation observed from astrophysical systems containing
relativistic jets and shocks e.g. gamma-ray bursts (GRBs) active galactic
nuclei (AGNs) and microquasars commonly exhibit power-law emission spectra.
Recent PIC simulations of relativistic electron-ion (or electron-positron) jets
injected into a stationary medium show that particle acceleration occurs within
the downstream jet. In collisionless relativistic shocks particle (electron,
positron and ion) acceleration is due to plasma waves and their associated
instabilities (e.g. the Weibel (filamentation) instability) created in the
shock region. The simulations show that the Weibel instability is responsible
for generating and amplifying highly non-uniform small-scale magnetic fields.
These fields contribute to the electron's transverse deflection behind the jet
head. The resulting ``jitter'' radiation from deflected electrons has different
properties compared to synchrotron radiation which assumes a uniform magnetic
field. Jitter radiation may be important for understanding the complex time
evolution and/or spectra in gamma-ray bursts, relativistic jets in general and
supernova remnants.Comment: 19 pages,7 figures, contributed talk at Seventh European Workshop on
Collisionless Shocks, Paris, 7- 9 November 2007. High resolution version can
be obtained at http://gammaray.nsstc.nasa.gov/~nishikawa/shockws07.pd
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