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1 FOREWARD The NRL Plasma Formulary originated over twenty five years ago and has been revised several times during this period. The guiding spirit and person primarily responsible for its existence is Dr. David Book. I am indebted to Dave for providing me with the T E X files for the Formulary and his continued suggestions for improvement. The Formulary(More)
Two-dimensional Hall magnetohydrodynamic simulations are used to determine the magnetic reconnection rate in the Hall limit. The simulations are run until a steady state is achieved for four initial current sheet thicknesses: L=1,5,10, and 20c/omega(pi), where c/omega(pi) is the ion inertial length. It is found that the asymptotic (i.e., time independent)(More)
Simulation results from the NRL ionospheric model SAMI2 indicate that the changes in the F-region over Millstone Hill during the geomagnetic storm beginning on 3 April 2004 are primarily due to the influence of a long-lasting eastward electric field, as was previously suggested by Huang et al. [2005]. A simulation of the storm day agrees well with the(More)
NASA OSS LWS TR&T-NNH05ZDA001N is a three-year program to develop techniques for accurate and precise estimation of solar surface flows from magnetogram data. Local Correlation Tracking (LCT) is the de-facto standard for estimating motion in solar image sequences. However, this technique has many documented limitations. Perhaps the greatest limitations of(More)
We present new analytical and numerical results of the dynamics of reversed field current layers in the Hall limit (i.e., characteristic length scales smaller than the ion inertial length). A rapid, localized thinning of the current layer leads to the generation of a nonlinear, shocklike structure that propagates in the B x inverted Delta(n) direction. This(More)
[1] The dynamics of x-line formation and evolution in 3D magnetic reconnection is studied using a fully kinetic approach. An x-line of small length is initialized using a perturbation localized in the current direction. The electrons and ions drift diamagnetically along the current direction of the initial x-line and are further accelerated by the(More)
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