Fast plasma sheet flows and X line motion in the Earth's magnetotail : results from a global hybrid-Vlasov simulation

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Juusola , L , Hoilijoki , S , Pfau-Kempf , Y , Ganse , U , Järvinen , R , Battarbee , M , Kilpua , E , Turc , L & Palmroth , M 2018 , ' Fast plasma sheet flows and X line motion in the Earth's magnetotail : results from a global hybrid-Vlasov simulation ' , Annales Geophysicae , vol. 36 , no. 5 , pp. 1183-1199 . https://doi.org/10.5194/angeo-36-1183-2018

Title: Fast plasma sheet flows and X line motion in the Earth's magnetotail : results from a global hybrid-Vlasov simulation
Author: Juusola, Liisa; Hoilijoki, Sanni; Pfau-Kempf, Yann; Ganse, Urs; Järvinen, Riku; Battarbee, Markus; Kilpua, Emilia; Turc, Lucile; Palmroth, Minna
Contributor: University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
Date: 2018-09-10
Language: eng
Number of pages: 17
Belongs to series: Annales Geophysicae
ISSN: 0992-7689
URI: http://hdl.handle.net/10138/246353
Abstract: Fast plasma flows produced as outflow jets from reconnection sites or X lines are a key feature of the dynamics in the Earth's magnetosphere. We have used a polar plane simulation of the hybrid-Vlasov model Vlasiator, driven by steady southward interplanetary magnetic field and fast solar wind, to study fast plasma sheet ion flows and related magnetic field structures in the Earth's magnetotail. In the simulation, lobe reconnection starts to produce fast flows after the increasing pressure in the lobes has caused the plasma sheet to thin sufficiently. The characteristics of the earthward and tailward fast flows and embedded magnetic field structures produced by multi-point tail reconnection are in general agreement with spacecraft measurements reported in the literature. The structuring of the flows is caused by internal processes: interactions between major X points determine the earthward or tailward direction of the flow, while interactions between minor X points, associated with leading edges of magnetic islands carried by the flow, induce local minima and maxima in the flow speed. Earthward moving flows are stopped and diverted duskward in an oscillatory (bouncing) manner at the transition region between tail-like and dipolar magnetic fields. Increasing and decreasing dynamic pressure of the flows causes the transition region to shift earthward and tailward, respectively. The leading edge of the train of earthward flow bursts is associated with an earthward propagating dipolarization front, while the leading edge of the train of tailward flow bursts is associated with a tailward propagating plasmoid. The impact of the dipolarization front with the dipole field causes magnetic field variations in the Pi2 range. Major X points can move either earthward or tailward, although tailward motion is more common. They are generally not advected by the ambient flow. Instead, their velocity is better described by local parameters, such that an X point moves in the direction of increasing reconnection electric field strength. Our results indicate that ion kinetics might be sufficient to describe the behavior of plasma sheet bulk ion flows produced by tail reconnection in global near-Earth simulations.
Subject: Magnetospheric physics
magnetospheric configuration and dynamics
plasma sheet
space plasma physics
numerical simulation studies
BURSTY BULK FLOWS
INTERPLANETARY MAGNETIC-FIELD
SUBSTORM CURRENT WEDGE
THEMIS OBSERVATIONS
ION DISTRIBUTIONS
TEARING MODE
RECONNECTION
VLASIATOR
MAGNETOSHEATH
FORESHOCK
115 Astronomy, Space science
114 Physical sciences
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