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We describe a systematic development of kinetic entropy as a diagnostic in fully kinetic particle-in-cell (PIC) simulations and use it to interpret plasma physics processes in heliospheric, planetary, and astrophysical systems. First, we calculate kinetic entropy in two forms—the "combinatorial" form related to the logarithm of the number of microstates per macrostate and the "continuous" form related to flnf, where f is the particle distribution function. We discuss the advantages and disadvantages of each and discuss subtleties about implementing them in PIC codes. Using collisionless PIC simulations that are two-dimensional in position space and three-dimensional in velocity space, we verify the implementation of the kinetic entropy diagnostics and discuss how to optimize numerical parameters to ensure accurate results. We show the total kinetic entropy is conserved to three percent in an optimized simulation of antiparallel magnetic reconnection. Kinetic entropy can be decomposed into a sum of a position space entropy and a velocity space entropy, and we use this to investigate the nature of kinetic entropy transport during collisionless reconnection. We find the velocity space entropy of both electrons and ions increases in time due to plasma heating during magnetic reconnection, while the position space entropy decreases due to plasma compression. This project uses collisionless simulations, so it cannot address physical dissipation mechanisms; nonetheless, the infrastructure developed here should be useful for studies of collisional or weakly collisional heliospheric, planetary, and astrophysical systems. Beyond reconnection, the diagnostic is expected to be applicable to plasma turbulence and collisionless shocks. [ABSTRACT FROM AUTHOR]

The outflow velocity of jets produced by collisionless magnetic reconnection is shown to be reduced by the ion exhaust temperature in fully kinetic particle in cell simulations and in situ satellite observations. We derive a scaling relationship for the outflow velocity based on the upstream Alfvén speed and the parallel ion exhaust temperature, which is verified in kinetic simulations and observations. The outflow speed reduction is shown to be due to the firehose instability criterion, and so, for large enough guide fields, this effect is suppressed and the outflow speed reaches the upstream Alfvén speed based on the reconnecting component of the magnetic field. [ABSTRACT FROM AUTHOR]

Introduces this issue as a special issue which is a collection of articles based on invited presentations at the 41st Annual Meeting of the Division of Plasma Physics (DPP) of the American Physical Society held in Seattle, Washington, in November 1999. Details of the program which involved several papers and a mini-conferences on Turbulence in the Interstellar Medium and Solar Wind, Plasma Propulsion Physics, Dusty Plasmas, and Computational Studies of Complexity in Turbulent Plasma; Coverage of a broad variety of research in plasma physics and highlighting of areas of intense interest and investigation, such as the basic physics of waves, instabilities, turbulence and transport and the properties of non-neutral plasmas and matter under very high pressures; Details of tutorial papers and presentations which are meant to be understood by non-experts.