Turbulent plasma transport across the Earth's low-latitude boundary layer

Abstract

The Kelvin-Helmholtz instability is a key process for the transport of solar wind plasma into the Earth's magnetosphere when the interplanetary magnetic field (IMF) is northward. Previous kinetic simulations for symmetric layers have demonstrated that the flow vortices compress the magnetopause current layer and induce magnetic reconnection, leading to the rapid streaming of solar wind plasma into the vortices along newly reconnected field lines. Using fully kinetic 3-D simulations, we demonstrate that the inherent density asymmetry across the boundary layer leads to a spectrum of oblique interchange instabilities along the magnetospheric side of the vortices. These secondary instabilities give rise to turbulence, which transports the solar wind plasma originally stored within the flow vortices deep into the magnetosphere. Simple estimates suggest that this turbulent transport may contribute significantly to the formation of the Earth's low-latitude boundary layer and the cold-dense plasma sheet during prolonged periods of northward IMF. Key PointsWe performed 3-D fully kinetic simulations modeling the Earth's magnetopauseThe KH instability drives turbulence leading to efficient solar wind transportThe estimated transport rate explains the formation of the LLBL and CDPS