Magnetotail Reconnection

Петрукович, А. А.; Artemyev, А. V.; Nakamura, R.

doi:10.1007/978-3-319-26432-5_7

Cited by 18 publications

(14 citation statements)

References 177 publications

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“…For example, observations by THEMIS and Cluster have enabled advances in our understanding of substorm dynamics and current sheet dynamics relevant to near-Earth magnetotail reconnection (e.g. reviews by Sergeev et al 2012;Petrukovich et al 2016). The newly launched MMS spacecraft have started to/will resolve the physical properties of near-Earth magnetotail reconnection and associated disturbances down to electron scales.…”

Section: Magnetotail Dynamicsmentioning

confidence: 99%

The Scientific Foundations of Forecasting Magnetospheric Space Weather

et al. 2017

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The magnetosphere is the lens through which solar space weather phenomena are focused and directed towards the Earth. In particular, the non-linear interaction of the solar wind with the Earth's magnetic field leads to the formation of highly inhomogenous electrical currents in the ionosphere which can ultimately result in damage to and problems with the operation of power distribution networks. Since electric power is the fundamental cornerstone of modern life, the interruption of power is the primary pathway by which space weather has impact on human activity and technology. Consequently, in the context of space weather, it is the ability to predict geomagnetic activity that is of key importance. This is usually stated in terms of geomagnetic storms, but we argue that in fact it is the substorm phenomenon which contains the crucial physics, and therefore prediction of substorm occurrence, severity and duration, either within the context of a longer-lasting geomagnetic storm, but potentially also as an isolated event, is of critical importance. Here we review the physics of the magnetosphere in the frame of space weather forecasting, focusing on recent results, current understanding, and an assessment of probable future developments.

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Section: Magnetotail Dynamicsmentioning

confidence: 99%

The Scientific Foundations of Forecasting Magnetospheric Space Weather

et al. 2017

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“…The spatial magnetic and plasma configuration of the magnetotail current sheet (CS) determine its stability properties (Lui, ; Petrukovich et al, ; Schindler, ) and thus control the onset of magnetospheric substorms, phenomena responsible for magnetic energy release, and energetic particle injections into the inner magnetosphere (Angelopoulos et al, ; Baker et al, ). This underlines the importance of observational investigations and modeling of the CS plasma and magnetic field configuration (see, e.g., reviews by Artemyev & Zelenyi, ; Lui, , and references therein).…”

Section: Introductionmentioning

confidence: 99%

Ion Anisotropy in Earth's Magnetotail Current Sheet: Multicomponent Ion Population

et al. 2019

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The configuration and stability of the magnetotail current sheet, which determine the dynamics of the entire magnetosphere, largely depend on the ion kinetics as inferred from the velocity distribution function. This distribution is shaped by various transient acceleration processes and by contributions from the ionosphere and the distant magnetotail. Investigating the ion distribution is thus crucially important for adequate modeling of the current sheet stability. This necessitates spacecraft observations of the ion distribution in a wide energy range, from ionospheric outflow energies (below 1 keV) to high energies (approximately hundreds of kiloelectron volts). Using combined measurements of Electrostatic Analyzer and Solid State Telescope onboard Time History of Events and Macroscale Interactions during Substorms in 2008–2009 tail seasons, we demonstrate that the ion distribution in the quiet magnetotail current sheet (at times devoid of fast plasma flows and large electric fields) consists of three populations: a subthermal field‐aligned anisotropic population (contributing ∼90% to the total density but only ∼20% to the total pressure), an isotropic thermal population (contributing ∼10% of the total density and ∼60% of the total pressure), and a transversely anisotropic suprathermal population (contributing <1% of the total density and ∼20% of the total pressure). The suprathermal population may include high‐energy ions moving along transient (Speiser) orbits. The competing effects of subthermal and suprathermal partial pressure anisotropies result in an almost isotropic total (combined) ion pressure. We characterize the dependence of the ion distribution characteristics, including the anisotropy of different populations on local plasma sheet activity (ion flows and electric fields). We discuss the implications of our results for current sheet modelling.

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“…Such a 3‐D configuration influences not only postreconnection (postdipolarization) convection but also CS stability. Because in the past, kinetic investigations of thin CS formation and subsequent destabilization were performed for 2‐D systems (see reviews by Artemyev & Zelenyi, ; Lui, ; Petrukovich et al, , and references therein), new kinetic models and simulations are needed to incorporate these 3‐D effects into a realistic scenario of magnetotail destabilization during the substorm growth phase.…”

Section: Discussionmentioning

confidence: 99%

“…Internally or externally driven instabilities of such CSs result in magnetic reconnection and the release of stored magnetic energy in the form of charged particle acceleration and plasma heating. Accelerated by magnetic field line stresses in CSs, plasma flows transport energetic particles to the inner magnetosphere, where they contribute to ring current formation and plasma wave generation (see more details in reviews by Birn, ; Petrukovich et al, ). Critical to this scenario is substorm onset, which is closely related to thin CS destruction by magnetic field dipolarization following magnetic reconnection.…”

Section: Introductionmentioning

confidence: 99%

Global View of Current Sheet Thinning: Plasma Pressure Gradients and Large‐Scale Currents

et al. 2019

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The formation of a thin magnetotail current sheet is a key process in magnetic energy accumulation before magnetic reconnection during substorms. Although the 3‐D configuration of a thinning current sheet has been well reproduced in many numerical simulations, observational details of this configuration have been less thoroughly studied. To investigate the global and local 3‐D structure of a thinning current sheet, we use a data set collected by three spacecraft of the Time History of Events and Macroscale Interactions during Substorms mission, two spacecraft of the Acceleration, Reconnection, Turbulence and Electrodynamics of Moon's Interaction with the Sun mission, and the Geostationary Operational Environmental Satellite 15. We demonstrate that near‐Earth current sheet thinning is accompanied by the formation of equatorial plasma pressure gradients directed from the flanks toward midnight. These gradients are associated with an intensification of the dawn‐dusk current (during current sheet thinning) and field‐aligned currents of opposite polarity at the dawn and dusk flanks. Simultaneous Time History of Events and Macroscale Interactions during Substorms and Acceleration, Reconnection, Turbulence and Electrodynamics of Moon's Interaction with the Sun observations show that current sheet thinning occupies a large portion of the tail, from the near‐Earth region to lunar orbit. An increase in the equatorial plasma pressure (and the lobe magnetic field pressure) is provided by a cold plasma density increase in the near‐Earth tail and likely by a plasma temperature increase in the distant tail. We discuss plasma convection patterns that are consistent with observed properties of the current sheet thinning.

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Magnetotail Reconnection

Cited by 18 publications

References 177 publications

The Scientific Foundations of Forecasting Magnetospheric Space Weather

The Scientific Foundations of Forecasting Magnetospheric Space Weather

Ion Anisotropy in Earth's Magnetotail Current Sheet: Multicomponent Ion Population

Global View of Current Sheet Thinning: Plasma Pressure Gradients and Large‐Scale Currents

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