Collisionless plasmas are a common feature of many astrophysical systems
(e.g. active galactic nuclei, supernova remnants, clusters of
(galaxies) and exhibit unique properties stemming from the loose coupling
between particle species and the plasma instabilities that can accelerate
some species efficiently and others not at all. Supernova remnant shocks
are efficient particle accelerators and may be responsible for the bulk of
cosmic rays below 1000 TeV. Galactic and Magellanic Cloud remnants are
close enough that the Chandra X-ray observatory has enabled us to spatially
resolve theshock heated material as it relaxes downstream. A complete picture of the
particle acceleration in collisionless shocks requires the examination of
the magnetic field, the thermal and cosmic raypopulations of protons, ion and electrons, and the dynamical effects of
magnetic field amplification and cosmic ray losses. In this talk I will
focus on the diagnostic capabilities of X-ray spectralobservations of the thermal plasma advecting away from the shock to
determine not only the initial electron heating at the shock front butalso to see the effects of the elusive cosmic-ray ions.
To begin viewing slides, click on the first slide below. (Or, view as pdf.)