Distant magnetotail reconnection and the coupling to the near‐Earth plasma sheet: Wind and Geotail case study

Øieroset, M.; Phan, T. D.; Fujimoto, M.; Lin, R. P.

doi:10.1029/2004gl020321

Cited by 9 publications

(5 citation statements)

References 21 publications

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“…From WIND data, Øieroset et al. (2000, 2004) reported five fast flow events occurring in the tail about 25–60 RE during a four‐day period with mainly northward IMF conditions. The analysis of these fast flows suggests that quasi steady reconnection can occur in the mid‐magnetotail region during periods of persistent northward IMF.…”

Section: Discussionmentioning

confidence: 99%

Magnetotail Configuration Under Northward IMF Conditions

et al. 2021

JGR Space Physics

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Due to the sparsity of space probes, it is still not clear on how the magnetic structure of the magnetotail looks like and how it evolves when the interplanetary magnetic field (IMF) directs northward. This simulation study uses two different global magnetosphere magnetohydrodynamics (MHD) models to simulate two northward IMF events and study the evolution of the magnetotail. Both models show that the magnetotail may form a structure that is composed of a dawnside tail lobe and a duskside tail lobe, under northward IMF conditions with significant By, instead of a northern tail lobe and a southern tail lobe under southward IMF conditions. In this magnetic configuration, a tail lobe extends a domain from northern (southern) cusp to southern (northern) IMF. The larger the magnitude of IMF clock angle, the longer and wider the magnetotail. Such magnetic configuration suggests that magnetotail reconnection is possible to occur when the dawnside tail lobe contacts with the duskside tail lobe and thus a substorm is also possible to occur under northward IMF conditions with significant By.

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Section: Discussionmentioning

confidence: 99%

Magnetotail Configuration Under Northward IMF Conditions

et al. 2021

JGR Space Physics

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“…The dawn‐dusk spatial localization of PSBL beamlets then seems to be very natural because as it was reported by Angelopoulos et al [1989], bursty bulk flows (BBFs), which are also the result of magnetotail reconnection and which may be considered as the CPS counterparts of PSBL beamlets, have a finite spatial extent (∼1–3 R E [ Sergeev et al , 1996; Angelopoulos et al , 1997; Kauristie et al , 2000; Nakamura et al , 2001, 2004a]). Recently, Oieroset et al [2004] provided experimental evidences that energization processes could have rather large duration (∼10 hours) and finite spread in dawn‐dusk direction (≥1 R E ).…”

Section: Introductionmentioning

confidence: 99%

Spatial‐Temporal characteristics of ion beamlets in the plasma sheet boundary layer of magnetotail

Григоренко

Sauvaud²,

Zelenyǐ

2007

J. Geophys. Res.

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[1] The processes of nonadiabatic ion acceleration occurring in the vicinity of magnetic neutral lines produce highly accelerated (up to 2500 km/s) field-aligned ion beams (beamlets) with transient appearance streaming earthward in the plasma sheet boundary layer (PSBL) of the Earth's magnetotail. Previous studies of these phenomena based on single spacecraft (s/c) missions supported the view that beamlets are temporal transients, since the typical time of a beamlet observation at a given s/c very rarely exceeds $1-2 min. Now multipoint Cluster observations have led to a new understanding of these phenomena with a spatial rather than a temporal structure. On the basis of 3-year Cluster measurements made in the PSBL, we present statistical evaluation of the beamlet duration (at least 5-15 min) and confirm well-manifested localization of the beamlet along Z and in some cases along Y directions, i.e., approximately across the lobe magnetic field. Earlier results reporting shorter beamlet observations could be understood by invoking not only PSBL flapping motions but also of an additional effect revealed by Cluster: earthward propagation of kink-like perturbations along the beamlet filaments. Phase velocity of these perturbations is of the order of the local Alfven velocity (V $ 600-1400 km/s) and related fast flappings of localized beamlet structures in the Y-Z direction significantly decreasing the time of their observation at a given spacecraft. Multipoint observations of beamlets revealed that they represent long-living ($5-15 min) plasma filaments elongated along the lobe magnetic field ($60-100R E ) and strongly localized in direction perpendicular to the PSBL-lobe boundary ($0.2-0.7R E ). In some cases, it was also possible to estimate the width of beamlet in dawn-dusk direction which was of the order of fractions of R E .Citation: Grigorenko, E. E., J.-A. Sauvaud, and L. M. Zelenyi (2007), Spatial-Temporal characteristics of ion beamlets in the plasma sheet boundary layer of magnetotail,

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“…Previous studies found that the asymptotic asymmetric conditions and the guide field are the two main factors determining Hall field patterns (Oieroset et al 2004;Cassak & Shay 2007;Cassak & Shay 2008;Mozer et al 2008;Pritchett 2008;Eastwood et al 2010). The asymptotic asymmetry and the guide field for the three events are listed in Table 1.…”

Section: Analyses and Discussionmentioning

confidence: 99%

“…The asymptotic asymmetry parameter (Phan & Paschmann 1996) is found to play an important role in determining the magnetic field and electric field pattern in the Hall effect (Oieroset et al 2004;Cassak & Shay 2007;Mozer et al 2008). In previous studies, the asymmetry is typically estimated using asymptotic (also called background) plasma parameters in the inflow regions of reconnection.…”

Section: Introductionmentioning

confidence: 99%

Hall Fields and Current Systems of Magnetic Reconnection under Asymmetric Conditions

Zhang

Tang

2023

ApJ

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The Hall effect is a key component of collisionless reconnection. A previous study showed that a quadrupolar Hall pattern under symmetric conditions degenerates into a bipolar pattern under highly asymmetric conditions. We study the properties of Hall magnetic fields and current systems during three reconnection events observed by the Magnetospheric Multiscale mission at the dayside magnetopause. Although the asymptotic density ratio between the magnetosheath and magnetospheric plasmas is very high for all three events, clear quadrupolar Hall field patterns are observed in all three events. The quadrupolar Hall magnetic fields in the three events display their respective properties on the intensity asymmetry and the distributing location. Among these events, a quadrupolar Hall field pattern is observed for the first time in in situ observations: the magnetosheath Hall pattern occupies the whole midplane region, while the magnetosphere Hall pattern still exists under highly asymmetric conditions. Observations show that the plasma mixture modulates the density asymmetry in the Hall region, which can be very different from the asymptotic density asymmetry in the magnetosheath and magnetospheric inflow plasma. The analyses indicate that the different density asymmetry inside the Hall region, but not the asymptotic density asymmetry, is an exact indicator that explains the different observed Hall patterns. Based on the observed facts, we suggest that the three reconnection events studied here are in different phases of their development after they are triggered under highly asymmetric conditions. Our results provide new insights into how the Hall effect works with the evolution of asymmetry during reconnection.

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Distant magnetotail reconnection and the coupling to the near‐Earth plasma sheet: Wind and Geotail case study

Cited by 9 publications

References 21 publications

Magnetotail Configuration Under Northward IMF Conditions

Magnetotail Configuration Under Northward IMF Conditions

Spatial‐Temporal characteristics of ion beamlets in the plasma sheet boundary layer of magnetotail

Hall Fields and Current Systems of Magnetic Reconnection under Asymmetric Conditions

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