Understanding magnetotail current sheet meso-scale structures using MHD simulations

Recent Cluster observations have strongly supported the existence of meso-scale structure in the magnetotail current sheet. In our study, a magnetohydrodynamic simulation event study exhibited current sheet behavior comparable to that seen in the Cluster observations. Geotail and DoubleStar observations also show that the simulation is providing a realistic representation of the magnetosphere during the period of interest; that is, when the current sheet evidently becomes bifurcated. The magnetohydrodynamic simulation allows us to place the local observations into a global contest. It shows that the observations can be explained in terms of localized reconnection tailward of the Cluster location and the formation of a flux rope nearby. The simulation also features wave-like structure across the current sheet.     

Mission-oriented theory for ISTP

The goal of mission-oriented theory is to develop techniques and models which can be used by experimentalists and theorists to interpret spacecraft measurements, deducing from them the maximum amount of information about both local and large-scale dynamics. To be effective, theorists and experimentalists must express their results in a common format. A reasonable starting point is for mission theorists to adopt the format currently used by experimentalists. To this end we have developed new diagnostics for plasma kinetic simulations, which display the results in formats very similar to those commonly used to present satellite wave and particle measurements. We have used a simulation of broadband electrostatic noise to demonstrate how, by comparing simulation results with observations, we can infer quantities which cannot be measured, such as the wave mode. We are also developing the capability of creating data streams from virtual spacecraft located in the simulation region. For example, we used a kinetic magnetopause simulation to explore the ways in which simulations can assist in the interpretation of single and multiple satellite measurements in regions of strong spatial inhomogeneity. To address directly the mission objective of measuring global transport, global MHD models are employed. In order to facilitate the initial comparison with ISTP satellites, time histories of simulated generic states of the magnetosphere will be stored on optical disks; these will then be used to create dynamical displays of both local parameters and the global configuration. Finally we demonstrate the use of data based phenomenological magnetic field models in single particle trajectory calculations to describe large-scale kinetic properties of the magnetospheric plasma. We briefly discuss the success of large-scale kinetic calculations in delineating the structure of the plasma sheet, and present some possible ISTP research initiatives which can be used to determine the structure of the very distant tail and the entry of plasma into the tail.     

Modeling PSBL high speed ion beams observed by Cluster and Double Star

On October 8, 2004, the Cluster and Double Star spacecraft crossed the near-Earth (12–19 R_E) magnetotail neutral sheet during the recovery phase of a small, isolated substorm. Although they were separated in distance by ∼7 R_E and in time by ∼30 min, both Cluster and Double Star observed steady, but highly structured Earthward moving >1000 km/s high speed H⁺ beams in the PSBL. This paper utilizes a global magnetohydrodynamic (MHD) simulation driven by Wind spacecraft solar wind input to model the large-scale structure of the PSBL and large-scale kinetic (LSK) particle tracing calculations to investigate the similarities and differences in the properties of the observed beams. This study finds that the large-scale shape of the PSBL is determined by the MHD configuration. On smaller scales, the LSK calculations, in good qualitative agreement with both Cluster and Double Star observations, demonstrated that the PSBL is highly structured in both time and space, on time intervals of less than 2 min, and spatial distances of the order of 0.2–0.5 R_E. This picture of the PSBL is different from the ordered and structured region previously reported in observations.