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

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Fast plasma sheet flows and X line motion in the Earth's magnetotail : Results from a global hybrid-Vlasov simulation. / Juusola, Liisa; Hoilijoki, Sanni; Pfau-Kempf, Yann; Ganse, Urs; Jarvinen, Riku; Battarbee, Markus; Kilpua, Emilia; Turc, Lucile; Palmroth, Minna.

In: Annales Geophysicae, Vol. 36, No. 5, 10.09.2018, p. 1183-1199.

Research output: Contribution to journalArticleScientificpeer-review

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Juusola, L, Hoilijoki, S, Pfau-Kempf, Y, Ganse, U, Jarvinen, 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

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Juusola, Liisa ; Hoilijoki, Sanni ; Pfau-Kempf, Yann ; Ganse, Urs ; Jarvinen, Riku ; Battarbee, Markus ; Kilpua, Emilia ; Turc, Lucile ; Palmroth, Minna. / Fast plasma sheet flows and X line motion in the Earth's magnetotail : Results from a global hybrid-Vlasov simulation. In: Annales Geophysicae. 2018 ; Vol. 36, No. 5. pp. 1183-1199.

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@article{2532cf152cbb4e2fa92733cec2e385a9,
title = "Fast plasma sheet flows and X line motion in the Earth's magnetotail: Results from a global hybrid-Vlasov simulation",
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.",
author = "Liisa Juusola and Sanni Hoilijoki and Yann Pfau-Kempf and Urs Ganse and Riku Jarvinen and Markus Battarbee and Emilia Kilpua and Lucile Turc and Minna Palmroth",
year = "2018",
month = "9",
day = "10",
doi = "10.5194/angeo-36-1183-2018",
language = "English",
volume = "36",
pages = "1183--1199",
journal = "Annales Geophysicae",
issn = "0992-7689",
publisher = "Copernicus Gesellschaft mbH",
number = "5",

}

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TY - JOUR

T1 - Fast plasma sheet flows and X line motion in the Earth's magnetotail

T2 - Results from a global hybrid-Vlasov simulation

AU - Juusola, Liisa

AU - Hoilijoki, Sanni

AU - Pfau-Kempf, Yann

AU - Ganse, Urs

AU - Jarvinen, Riku

AU - Battarbee, Markus

AU - Kilpua, Emilia

AU - Turc, Lucile

AU - Palmroth, Minna

PY - 2018/9/10

Y1 - 2018/9/10

N2 - 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.

AB - 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.

UR - http://www.scopus.com/inward/record.url?scp=85053221370&partnerID=8YFLogxK

U2 - 10.5194/angeo-36-1183-2018

DO - 10.5194/angeo-36-1183-2018

M3 - Article

VL - 36

SP - 1183

EP - 1199

JO - Annales Geophysicae

JF - Annales Geophysicae

SN - 0992-7689

IS - 5

ER -

ID: 28137205