The formation of superdense plasma sheet in association with the IMF turning from northward to southward

Li, Wenhui; Raeder, J.; Thomsen, M. F.; Lavraud, B.; Lu, Liying; Liang, En‐Wei

doi:10.1002/2016ja023373

Cited by 7 publications

(6 citation statements)

References 86 publications

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“…The ion spectrum features two ion populations with distinctly different energies (Figure2h), whose cold and hot ion population energies are ~1 keV and ~3 keV, respectively. These features are consistent with those in the CDPS[10,35,[51][52][53][54], which is widely believed to be the consequence of the solar wind entry[12,51,52]. During the crossing of the CDPS (10:10:00-11:50:00 UT), the temperature of the cold ion populations was ~400 eV (green curve in Figure2d), while that of the hot ion populations was ~11,500 eV (blue curve in Figure2d).…”

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confidence: 85%

Cold and Dense Plasma Sheet Caused by Solar Wind Entry: Direct Evidence

Chen

2020

Atmosphere

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We present a coordinated observation with the Magnetospheric Multiscale (MMS) mission, located in the Earth’s magnetotail plasma sheet, and the Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon’s Interaction with the Sun (ARTEMIS) mission, located in the solar wind, in order to understand the formation mechanism of the cold and dense plasma sheet (CDPS). MMS detected two CDPSs composed of two ion populations with different energies, where the energy of the cold ion population is the same as that of the solar wind measured by ARTEMIS. This feature directly indicates that the CDPSs are caused by the solar wind entry. In addition, He+ was observed in the CDPSs. The plasma density in these two CDPSs are ~1.8 cm−3 and ~10 cm−3, respectively, roughly 4–30 times the average value of a plasma sheet. We performed a cross-correlation analysis on the ion density of the CDPS and the solar wind, and we found that it takes 3.7–5.9 h for the solar wind to enter the plasma sheet. Such a coordinated observation confirms the previous speculation based on single-spacecraft measurements.

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confidence: 85%

Cold and Dense Plasma Sheet Caused by Solar Wind Entry: Direct Evidence

Chen

2020

Atmosphere

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“…OpenGGCM can also be coupled with an inner magnetosphere model. It has been used in simulating some events with well agreement with observations, especially for events under NIMF conditions (Li et al, 2005(Li et al, , 2009(Li et al, , 2017.…”

Section: Simulation Resultsmentioning

confidence: 99%

The Dawn‐Dusk Tail Lobe Magnetotail Configuration and the Formation of Aurora Transpolar Arc

Angelopoulos

Mieth

et al. 2022

JGR Space Physics

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Most of the disturbances in space environment can be explained under the framework theory of open magnetosphere and Dungey cycle (Dungey, 1961). This theory is sketched in Figure 1 which is similar to Dungey's original figure. Under southward IMF (SIMF) conditions, magnetic reconnection occurs first at the nose of the magnetopause (Figure 1c) where IMF field lines interconnect with dayside geomagnetic closed field lines. Such reconnection creates a northern set and a southern set of open field lines that consequently convect toward nightside and form into a north-south tail lobe magnetotail configuration (Figures 1a and 1b). Then the northern open field lines interconnect with the southern open field lines in the tail (Figure 1d), creating new closed field lines and new IMF field lines. These two magnetic reconnection processes thus form a Dungey cycle, during which the topology of involved geomagnetic field lines changes from closed to open in dayside and then changes back from open to closed in nightside. This cycle causes solar wind mass and energy to enter into the magnetosphere and the ionosphere, resulting in disturbances such as magnetic storm, substorm, aurora, and so on.

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“…One is the BATS‐R‐US which has been chosen by NOAA Space Weather Prediction Center to be part of the operational space weather model. The other is the OpenGGCM which has been used in simulating some events with well agreement with observations, especially for events under northward IMF conditions (Li et al., 2005, 2009, 2017; Raeder et al., 1995).…”

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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The formation of superdense plasma sheet in association with the IMF turning from northward to southward

Cited by 7 publications

References 86 publications

Cold and Dense Plasma Sheet Caused by Solar Wind Entry: Direct Evidence

Cold and Dense Plasma Sheet Caused by Solar Wind Entry: Direct Evidence

The Dawn‐Dusk Tail Lobe Magnetotail Configuration and the Formation of Aurora Transpolar Arc

Magnetotail Configuration Under Northward IMF Conditions

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