We present a simple model of nonlinear diffusive shock acceleration (also called first-order Fermi shock acceleration) that determines the shock modification, spectrum, and efficiency of the process in the plane-wave, steady state approximation as a function of an arbitrary injection parameter, η. The model, which uses a three-power-law form for the accelerated particle spectrum and contains only simple algebraic equations, includes the essential elements of the full nonlinear model and has been tested against Monte Carlo and numerical kinetic shock models. We include both adiabatic and Alfven wave heating of the upstream precursor. The simplicity and ease of calculation make this model useful for studying the basic properties of nonlinear shock acceleration, as well as providing results accurate enough for many astrophysical applications. It is shown that the shock properties depend upon the shock speed u0 with respect to a critical value u ηp, which is a function of the injection rate η and maximum accelerated particle momentum pmax. For u0 MA0, or by rtot ≈ 1.5M in the opposite case (MS0 is the sonic Mach number and MA0 is the Alfven Mach number). If u0 > u, the shock, although still strong, becomes almost unmodified and accelerated particle production decreases inversely proportional to u0.

https://iopscience.iop.org/article/10.1086/307993/pdf

A Simple Model of Nonlinear Diffusive Shock Acceleration

We have used archival ROSAT data to present X-ray images of 31 supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). We have classified these remnants according to their X-ray morphologies, into the categories of shell-type, diffuse face, centrally brightened, point-source-dominated, and irregular. We suggest possible causes of the X-ray emission for each category and for individual features of some of the SNRs.

Supernova Remnants in the Magellanic Clouds. III. An X-Ray Atlas of Large Magellanic Cloud Supernova Remnants

We have used archival ROSAT data to present X-ray images of thirty-one supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) We have classified these remnants according to their X-ray morphologies, into the categories of Shell-Type, Diffuse Face, Centrally Brightened, Point-Source Dominated, and Irregular We suggest possible causes of the X-ray emission for each category, and for individual features of some of the SNRs

Supernova Remnants in the Magellanic Clouds III: An X-ray Atlas of LMC Supernova Remnants

Cosmic-ray energetics and mass (CREAM) balloon experiment

We present the scientific motivation and design for a Long Wavelength Array (LWA) to open a new, high resolution window on the electromagnetic spectrum from 15 - 150 MHz. This region has been poorly explored because ionospheric turbulence has limited imaging to very course angular resolution. New phase compensation techniques now make it possible to explore this region at unprecedented angular resolution. We describe a large (greater than 100 km), completely electronic instrument capable of imaging radio sources across the sky and spectrum rapidly, but which could be built at a fraction of the cost of higher frequency systems of comparable size or sophistication. The LWA will be a powerful instrument for delineating the interaction between nonthermal emitting plasmas and thermal absorbing gas, for differentiating between self-absorption processes, and for exploring the universe for coherent emission processes. For both Galactic and extragalactic work it will provide unique information on the distribution of ionized gas, relativistic particles, and magnetic fields. For solar physics the LWA will be the ideal solar radar receiver and can be used to image Earth-ward bound Coronal Mass Ejections for accurate geomagnetic storm prediction.

Meter- and decameter-wavelength array for astrophysics and solar radar

This paper reports on a Workshop on Supernova Remnants and the Physics of Strong Shock Waves hosted by North Carolina State University at Raleigh, North Carolina, September 16-18, 1993. The workshop brought together observers, shock theorists, cosmic-ray specialists, and simulators to address the role supernova remnants (SNRs) can play in furthering our understanding of the complex plasma physics associated with collisionless shocks and particle acceleration. Over fifty scientists presented papers on various aspects of supernova remnants. In lieu of a proceedings volume, we present here a synopsis of the workshop, in the form of brief summaries of each workshop session.

Supernova remnants and the physics of strong shock waves

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Supernova remnants and the physics of strong shock waves