Estimating Proximity to the Asymmetric Reconnection X-line

Magnetic reconnection is a process that changes magnetic topology, allows plasma transport across boundaries, and converts field potential energy to particle kinetic energy. All of these processes are tied to the X-line, or site of reconnection, yet current methods of locating the reconnection site either do not uniquely identify the the X-line or have not been tested when asymmetries in field strength and plasma density and temperature are present. Furthermore, identification of spacial structures (such as the X-line) as they traverse satellites is limited by hardware constraints. This thesis proposes a new method of locating the reconnection site for asymmetric magnetic reconnection (AMR), and an algorithm for merging fluxgate and searchcoil magnetometer datasets to improve data fidelity in a specific frequency range. Cluster observations show that asymmetries present during reconnection cause a variety of transitions in the reconnecting component of the magnetic field, ion density, ion outflow jets, and the normal component of the electric field across the magnetopause. Simulations in 2D and 3D and a laboratory experiment, both with and without guide field, contain similar offsets. Only within 5 electron inertial lengths of the X-line do transitions occur simultaneously. Farther away, transitions offset from one another in a systematic way. Electron distribution functions serve as an independent check of the method, as they take on a triangular shape that is unique to the X-line. Normal electric field offsets and outflow upstream from the X-line are linked to the presence of a guide field. This new methodology is applied to Cluster AMR events to demonstrate its use. One Cluster event in close proximity to the X-line exhibits triangle-shaped distributions and enhanced currents

Clustering of Global Magnetospheric Observations

The use of supervised methods in space science have demonstrated powerful capability in classification tasks, but unsupervised methods have been less utilized for the clustering of spacecraft observations. We use a combination of unsupervised methods, being principal component analysis, self-organizing maps, and hierarchical agglomerative clustering, to make predictions on if THEMIS and MMS observations occurred in the magnetosphere, magnetosheath, or the solar wind. The resulting predictions are validated visually by analyzing the distribution of predictions and studying individual time series. Particular nodes in the self organizing map are studied to see what data they represent. The capability of deeper hierarchical analysis using this model is briefly explored. Finally, the changes in region prediction can be used to infer magnetopause and bow shock crossings, which can act as an additional method of validation, and are saved for their utility in solar wind validation, understanding magnetopause processes, and the potential to develop a bow shock model.Comment: 36 pages, 22 figure

Quantifying Energy Conversion in Higher Order Phase Space Density Moments in Plasmas

Weakly collisional and collisionless plasmas are typically far from local thermodynamic equilibrium (LTE), and understanding energy conversion in such systems is a forefront research problem. The standard approach is to investigate changes in internal (thermal) energy and density, but this omits energy conversion that changes any higher order moments of the phase space density. In this study, we calculate from first principles the energy conversion associated with all higher moments of the phase space density for systems not in LTE. Particle-in-cell simulations of collisionless magnetic reconnection reveal that energy conversion associated with higher order moments can be locally significant. The results may be useful in numerous plasma settings, such as reconnection, turbulence, shocks, and wave-particle interactions in heliospheric, planetary, and astrophysical plasmas.Comment: 16 pages, 3 figures, includes both main paper and supplementary materia

Higher-order nonequilibrium term: Effective power density quantifying evolution towards or away from local thermodynamic equilibrium

A common approach to assess the nature of energy conversion in a classical fluid or plasma is to compare power densities of the various possible energy conversion mechanisms. A forefront research area is quantifying energy conversion for systems that are not in local thermodynamic equilibrium (LTE), as is common in a number of fluid and plasma systems. Here, we introduce the ``higher-order non-equilibrium term'' (HORNET) effective power density that quantifies the rate of change of departure of a phase space density from LTE. It has dimensions of power density, which allows for quantitative comparisons with standard power densities. We employ particle-in-cell simulations to calculate HORNET during two processes, namely magnetic reconnection and decaying kinetic turbulence in collisionless magnetized plasmas, that inherently produce non-LTE effects. We investigate the spatial variation of HORNET and the time evolution of its spatial average. By comparing HORNET with power densities describing changes to the internal energy (pressure dilatation, $\rm{Pi-D}$, and divergence of the vector heat flux density), we find that HORNET can be a significant fraction of these other measures (8\% and 35\% for electrons and ions, respectively, for reconnection; up to 67\% for both electrons and ions for turbulence), meaning evolution of the system towards or away from LTE can be dynamically important. Applications to numerous plasma phenomena are discussed.Comment: 19 pages (including references), 7 figure

Turbulence properties and kinetic signatures of electron in Kelvin-Helmholtz waves during a geomagnetic storm

We present a comprehensive study of Magnetospheric Multiscale (MMS) spacecraft encounter with KHI during a geomagnetic storm, focusing on elucidating key turbulence properties and reconnection signatures observed at the edges of KH vortices. The spectral slope for electric field stays approximately constant for frequencies below the ion cyclotron frequency and exhibits a break around the lower hybrid frequency, indicating wave activity. Furthermore, MMS observes a current sheet accompanied by intense electron jets and features consistent with strong guide-field asymmetric reconnection across the magnetopause. Substantial agyrotropy (by a factor of 10) in electron distribution functions is observed in the reconnecting current sheet and at the edges of KH. Our observation presents a multi-scale view into KH turbulence under strongly driven conditions and into the dynamics occurring at electron dissipation scales.Comment: 10 pages, including 4 figure

Electron inflow velocities and reconnection rates at earth's magnetopause and magnetosheath

Electron inflow and outflow velocities during magnetic reconnection at and near the dayside magnetopause are measured using satellites from NASA's Magnetospheric Multiscale (MMS) mission. A case study is examined in detail, and three other events with similar behavior are shown, with one of them being a recently published electron-only reconnection event in the magnetosheath. The measured inflow speeds of 200–400 km/s imply dimensionless reconnection rates of 0.05–0.25 when normalized to the relevant electron Alfvén speed, which are within the range of expectations. The outflow speeds are about 1.5–3 times the inflow speeds, which is consistent with theoretical predictions of the aspect ratio of the inner electron diffusion region. A reconnection rate of 0.04 ± 25% was obtained for the case study event using the reconnection electric field as compared to the 0.12 ± 20% rate determined from the inflow velocity.publishedVersio

HelioSwarm: A Multipoint, Multiscale Mission to Characterize Turbulence

HelioSwarm (HS) is a NASA Medium-Class Explorer mission of the Heliophysics Division designed to explore the dynamic three-dimensional mechanisms controlling the physics of plasma turbulence, a ubiquitous process occurring in the heliosphere and in plasmas throughout the universe. This will be accomplished by making simultaneous measurements at nine spacecraft with separations spanning magnetohydrodynamic and sub-ion spatial scales in a variety of near-Earth plasmas. In this paper, we describe the scientific background for the HS investigation, the mission goals and objectives, the observatory reference trajectory and instrumentation implementation before the start of Phase B. Through multipoint, multiscale measurements, HS promises to reveal how energy is transferred across scales and boundaries in plasmas throughout the universe

Seven Sisters: a mission to study fundamental plasma physical processes in the solar wind and a pathfinder to advance space weather prediction

This paper summarizes the Seven Sisters solar wind mission concept and the outstanding science questions motivating the mission science objectives. The Seven Sisters mission includes seven individual spacecraft designed to uncover fundamental physical processes in the solar wind and provides up to ≈ 2 days of advanced space weather warnings for 550 Earth days during the mission. The mission will collect critical measurements of the thermal and suprathermal plasma and magnetic fields, utilizing, for the first time, Venus–Sun Lagrange points. The multi-spacecraft configuration makes it possible to distinguish between spatial and temporal changes, define gradients, and quantify cross-scale transport in solar wind structures. Seven Sisters will determine the 3-D structure of the solar wind and its transient phenomena and their evolution in the inner heliosphere. Data from the Seven Sisters mission will allow the identification of physical processes and the quantification of the relative contribution of different mechanisms responsible for suprathermal particle energization in the solar wind

A New Theory of Kinetic-Scale Energy Conversion and Dissipation

The Magnetospheric Multiscale (MMS) mission has enabled research into kinetic-scale energy conversion and dissipation in exquisite detail. Studying energy conversion is complicated where collisions are extremely weak, leading to systems far from local thermodynamic equilibrium (LTE). Recently, the crucial role played by non-LTE effects in impacting the evolution of plasma temperature has been emphasized [Y. Yang et al., Phys. Plasmas, 24, 072306 (2017)]. The key non-LTE term is known as Pi-D, which appears in the temperature evolution equation. In this study, we show the temperature evolution equation is incomplete, missing key kinetic physics that can play an important role in energy conversion. We argue that energy conversion can be thought of as a hierarchy of changes to all moments of the phase space density. Work due to compression changes the zeroth moment (density), while Pi-D and heat flux change the second moment (temperature); both are described by the temperature evolution equation. However, the equation is agnostic to changes to any higher order moment. We develop a new paradigm to describe these manifestly non-LTE kinetic effects. Using entropy defined in kinetic theory, we derive an energy evolution equation that supplants the first law of thermodynamics – we dub it “the first law of kinetic theory.” We show this law retains all information described by the temperature evolution equation, in addition to describing energy conversion to all higher order moments. We compare and contrast amplitudes and profiles of terms in the first law of kinetic theory in particle-in-cell simulations of symmetric magnetic reconnection