363 research outputs found
Index
The interest in relativistic beam-plasma instabilities has been greatly rejuvenated over the past two decades by novel concepts in laboratory and space plasmas. Recent advances in this long-standing field are here reviewed from both theoretical and numerical points of view. The primary focus is on the two-dimensional spectrum of unstable electromagnetic waves growing within relativistic, unmagnetized, and uniform electron beam-plasma systems. Although the goal is to provide a unified picture of all instability classes at play, emphasis is put on the potentially dominant waves propagating obliquely to the beam direction, which have received little attention over the years. First, the basic derivation of the general dielectric function of a kinetic relativistic plasma is recalled. Next, an overview of two-dimensional unstable spectra associated with various beam-plasma distribution functions is given. Both cold-fluid and kinetic linear theory results are reported, the latter being based on waterbag and Maxwell–Jüttner model distributions. The main properties of the competing modes (developing parallel, transverse, and oblique to the beam) are given, and their respective region of dominance in the system parameter space is explained. Later sections address particle-in-cell numerical simulations and the nonlinear evolution of multidimensional beam-plasma systems. The elementary structures generated by the various instability classes are first discussed in the case of reduced-geometry systems. Validation of linear theory is then illustrated in detail for large-scale systems, as is the multistaged character of the nonlinear phase. Finally, a collection of closely related beam-plasma problems involving additional physical effects is presented, and worthwhile directions of future research are outlined.Original Publication: Antoine Bret, Laurent Gremillet and Mark Eric Dieckmann, Multidimensional electron beam-plasma instabilities in the relativistic regime, 2010, Physics of Plasmas, (17), 12, 120501-1-120501-36. http://dx.doi.org/10.1063/1.3514586 Copyright: American Institute of Physics http://www.aip.org/</p
Diffusive Shock Acceleration with Magnetic Amplification by Non-resonant Streaming Instability in SNRs
We investigate the diffusive shock acceleration in the presence of the
non-resonant streaming instability introduced by Bell (2004). The numerical MHD
simulations of the magnetic field amplification combined with the analytical
treatment of cosmic ray acceleration permit us to calculate the maximum energy
of particles accelerated by high-velocity supernova shocks. The estimates for
Cas A, Kepler, SN1006, and Tycho historical supernova remnants are given. We
also found that the amplified magnetic field is preferentially oriented
perpendicular to the shock front downstream of the fast shock. This explains
the origin of the radial magnetic fields observed in young supernova remnants.Comment: 18 pages, 9 figures, accepted to Ap
High energy cosmic-rays: puzzles, models, and giga-ton neutrino telescopes
The existence of cosmic rays of energies exceeding 10^20 eV is one of the
mysteries of high energy astrophysics. The spectrum and the high energy to
which it extends rule out almost all suggested source models. The challenges
posed by observations to models for the origin of high energy cosmic rays are
reviewed, and the implications of recent new experimental results are
discussed. Large area high energy cosmic ray detectors and large volume high
energy neutrino detectors currently under construction may resolve the high
energy cosmic ray puzzle, and shed light on the identity and physics of the
most powerful accelerators in the universe.Comment: 12 pages, 7 figures; Summary of review talk, PASCOS 03 (Mumbai,
India
Nonthermal Emission from a Supernova Remnant in a Molecular Cloud
In evolved supernova remnants (SNRs) interacting with molecular clouds, such
as IC 443, W44, and 3C391, a highly inhomogeneous structure consisting of a
forward shock of moderate Mach number, a cooling layer, a dense radiative shell
and an interior region filled with hot tenuous plasma is expected. We present a
kinetic model of nonthermal electron injection, acceleration and propagation in
that environment and find that these SNRs are efficient electron accelerators
and sources of hard X- and gamma-ray emission. The energy spectrum of the
nonthermal electrons is shaped by the joint action of first and second order
Fermi acceleration in a turbulent plasma with substantial Coulomb losses.
Bremsstrahlung, synchrotron, and inverse Compton radiation of the nonthermal
electrons produce multiwavelength photon spectra in quantitative agreement with
the radio and the hard emission observed by ASCA and EGRET from IC 443. We
distinguish interclump shock wave emission from molecular clump shock wave
emission accounting for a complex structure of molecular cloud. Spatially
resolved X- and gamma- ray spectra from the supernova remnants IC 443, W44, and
3C391 as might be observed with BeppoSAX, Chandra XRO, XMM, INTEGRAL and GLAST
would distinguish the contribution of the energetic lepton component to the
gamma-rays observed by EGRET.Comment: 14 pages, 4 figure, Astrophysical Journal, v.538, 2000 (in press
How Can Schools Support Parents' Engagement in their Children's Learning? Evidence from Research and Practice
This is the final version. Available from the Education Endowment Foundation via the link in this recordEducation Endowment Foundatio
A multifrequency study of giant radio sources-II. Spectral ageing analysis of the lobes of selected sources
Multifrequency observations with the GMRT and the VLA are used to determine
the spectral breaks in consecutive strips along the lobes of a sample of
selected giant radio sources (GRSs) in order to estimate their spectral ages.
The maximum spectral ages estimated for the detected radio emission in the
lobes of our sources range from 6 to 36 Myr with a median value of
20 Myr using the classical equipartition fields. Using the magnetic field
estimates from the Beck & Krause formalism the spectral ages range from 5
to 38 Myr with a median value of 22 Myr. These ages are significantly
older than smaller sources. In all but one source (J1313+6937) the spectral age
gradually increases with distance from the hotspot regions, confirming that
acceleration of the particles mainly occurs in the hotspots. Most of the GRSs
do not exhibit zero spectral ages in the hotspots, as is the case in earlier
studies of smaller sources. This is likely to be largely due to contamination
by more extended emission due to relatively modest resolutions. The injection
spectral indices range from 0.55 to 0.88 with a median value of
0.6. We discuss these values in the light of theoretical expectations,
and show that the injection spectral index appears to be correlated with
luminosity and/or redshift as well as with linear size.Comment: 12 Pages, 13 Figures, 9 Tables, Accepted for publication in MNRA
Nonthermal Electrons at High Mach Number Shocks: Electron Shock Surfing Acceleration
We study the suprathermal electron acceleration mechanism in a perpendicular
magnetosonic shock wave in a high Mach number regime by using a
particle-in-cell simulation. We find that shock surfing/surftron acceleration
producing the suprathermal electrons occurs in the shock transition region
where a series of large amplitude electrostatic solitary waves (ESWs) are
excited by Buneman instability under the interaction between the reflected ions
and the incoming electrons. It is shown that the electrons are likely to be
trapped by ESWs, and during the trapping phase they can be effectively
accelerated by the shock motional/convection electric field. We discuss that
suprathermal electrons can be accelerated up to , where is the ion rest mass energy and is the shock upstream flow velocity.
Furthermore, some of these suprathermal electrons may be effectively trapped
for infinitely long time when Alfv\'en Mach number exceeds several 10,
and they are accelerated up to the shock potential energy determined by the
global shock size.Comment: 21 pages, 6 figure
Solar interacting protons versus interplanetary protons in the core plus halo model of diffusive shock acceleration and stochastic re-acceleration
With the first observations of solar γ-rays from the decay of pions, the relationship of protons producing ground level enhancements (GLEs) on the Earth to those of similar energies producing the γ-rays on the Sun has been debated. These two populations may be either independent and simply coincident in large flares, or they may be, in fact, the same population stemming from a single accelerating agent and jointly distributed at the Sun and also in space. Assuming the latter, we model a scenario in which particles are accelerated near the Sun in a shock wave with a fraction transported back to the solar surface to radiate, while the remainder is detected at Earth in the form of a GLE. Interplanetary ions versus ions interacting at the Sun are studied for a spherical shock wave propagating in a radial magnetic field through a highly turbulent radial ray (the acceleration core) and surrounding weakly turbulent sector in which the accelerated particles can propagate toward or away from the Sun. The model presented here accounts for both the first-order Fermi acceleration at the shock front and the second-order, stochastic re-acceleration by the turbulence enhanced behind the shock. We find that the re-acceleration is important in generating the γ-radiation and we also find that up to 10% of the particle population can find its way to the Sun as compared to particles escaping to the interplanetary space
Review of evidence on implementation in education
This is the final version. Available from the Education Endowment Foundation via the link in this recordBackground
‘Implementation in education’ refers to active and planned efforts to introduce and sustain an approach in schools. It
therefore involves making, and acting on, evidence-informed decisions. There is substantial evidence indicating that
quality implementation amplifies the effectiveness of a range of school-based approaches. However, implementation in
schools is complex and there is a need to know more about how to do implementation in schools well. It is important to
understand how new approaches can be selected and put in place in school settings to improve outcomes for all pupils,
including those from more disadvantaged backgrounds. There have been few reviews of research to date that take a
holistic view of implementation across multiple intervention and school types. The EEF commissioned this evidence
review to underpin an update to its guidance report ‘Putting Evidence to Work: A School’s Guide to Implementation’.
Aims of the evidence review
The evidence review aims to address two overarching questions:
1. How should school leaders and teachers understand implementation and how should they implement evidence informed approaches in their context to have the best chance of improving all pupils’ outcomes?
2. What is the relationship between content (‘what’) and process (‘how’) within school implementation?
To address these two questions the evidence review is organised into four inter-related ‘work packages’. Because
schools are complex, adaptive systems involving a diverse range of individuals, investigating implementation in schools
needs to focus on context to understand what works for whom, where, and why. This realist perspective is reflected in our approach throughout
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