Structure and dynamics of the magnetopause and its boundary layers

TL;DR

This paper reviews recent advances in understanding Earth's magnetopause structure and dynamics, emphasizing multi-spacecraft observations, plasma processes like reconnection and Kelvin-Helmholtz instability, and their implications for solar wind-magnetosphere interactions.

Contribution

It provides a comprehensive overview of magnetopause boundary layer processes, highlighting new visualization techniques and observational insights into magnetic reconnection and plasma transport mechanisms.

Findings

Magnetopause reconnection can be globally continuous under various IMF conditions.

Kelvin-Helmholtz instability can grow nonlinearly, inducing vortex reconnection.

Reconnection tailward of polar cusps is a key plasma entry mechanism.

Abstract

The magnetopause is the key region in space for the transfer of solar wind mass, momentum, and energy into the magnetosphere. During the last decade, our understanding of the structure and dynamics of Earth's magnetopause and its boundary layers has advanced considerably; thanks largely to the advent of multi-spacecraft missions such as Cluster and THEMIS. Moreover, various types of physics-based techniques have been developed for visualizing two- or three-dimensional plasma and field structures from data taken by one or more spacecraft, providing a new approach to the analysis of the spatiotemporal properties of magnetopause processes, such as magnetic reconnection and the Kelvin-Helmholtz instability (KHI). Information on the size, shape, orientation, and evolution of magnetic flux ropes or flow vortices generated by those processes can be extracted from in situ measurements. Observations show that magnetopause reconnection can be globally continuous for both southward and northward interplanetary magnetic field (IMF) conditions, but even under such circumstances, more than one X-line may exist within a certain (low-latitude or high-latitude) portion on the magnetopause and some X-lines may retreat anti-sunward. The potential global effects of such behavior are discussed. An overview is also given of the identification, excitation, evolution, and possible consequences of the magnetopause KHI: there is evidence for nonlinear KHI growth and associated vortex-induced reconnection under northward IMF. Observation-based estimates indicate that reconnection tailward of both polar cusps can be the dominant mechanism for solar wind plasma entry into the dayside magnetosphere under northward IMF. However, the mechanism by which the transferred plasma is transported into the central portion of the magnetotail, and the role of magnetopause processes in this transport remain unclear.