Equatorial distributions of the plasma sheet ions, their electric and magnetic drifts, and magnetic fields under different interplanetary magnetic field Bz conditions

Wang, Chih‐Ping; Lyons, L. R.; Weygand, J. M.; Nagai, T.; McEntire, R. W.

doi:10.1029/2005ja011545

Cited by 83 publications

(136 citation statements)

References 25 publications

(33 reference statements)

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“…The tendency for a component of the bulk flow to point away from midnight has been noted previously [Kaufmann et al, 2001;Wang et al, 2006]. This behavior suggests a source of plasma near midnight associated with flow toward the neutral sheet from the outer plasma sheet and the subsequent flow away from midnight in the neutral sheet.…”

Section: Energy Transport Sorted By F Cmentioning

confidence: 76%

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Ion heat flux and energy transport near the magnetotail neutral sheet

Kaufmann

Paterson

2008

J. Geophys. Res.

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[1] Ten-year averages of energy transport rates near the neutral sheet showed that the enthalpy flux density or thermal energy term Q T = (5/2)PV was the largest, where P is the isotropic pressure and V is the bulk flow velocity. The ion heat flux, q i , was the next largest term. Sorting data using a magnetic flux transport parameter showed that q i could become dominant during periods of slow flow. Both q i and the ion bulk velocity V i were duskward on the dusk side of the neutral sheet. This relationship is characteristic of crosstail drift and a heat flux that can be attributed to the energy dependent gradient and curvature drifts. The q i and V i vectors often pointed in different directions on the dawn side. The x component of q i on the dawn side pointed tailward, suggesting entry through the magnetopause of a suprathermal ion component. On the dusk side the q ix plots that were sorted using a magnetic flux transport parameter showed evidence of plasma sheet reconnection. The long-term averaged x component of Q T pointed earthward almost everywhere in the neutral sheet, and was attributed to periods of very fast plasma flow. The cross-tail component of Q T was separated into two contributions. One part of Q Ty involved a common drift away from midnight during both earthward and tailward fast flows. This feature suggests that thermal energy and plasma flow from the outer plasma sheet toward the neutral sheet near midnight, and then toward the flanks. The other part of Q Ty involved a differential duskward drift during fast earthward flows and a dawnward drift during fast tailward flows. The incremental E fields that would produce such convection point tailward during the fastest earthward flows and earthward during the fastest tailward flows. The dependencies of V i , q i and Q T on the interplanetary magnetic field (IMF) clock angle also were studied. Both V i and Q T were reduced when the IMF was northward and the neutral sheet plasma became cold and dense. However, no dependence of q i on the IMF direction was seen. This shows that the generation of a cold dense plasma sheet does not substantially change the distribution of the suprathermal ions that are most important in the production of q i .Citation: Kaufmann, R. L., and W. R. Paterson (2008), Ion heat flux and energy transport near the magnetotail neutral sheet,

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Section: Energy Transport Sorted By F Cmentioning

confidence: 76%

“…[40] The average ion density n i and temperature T i showed the well-known tendency for the plasma sheet to be cold and dense when the IMF was northward [Terasawa et al, 1997;Fujimoto et al, 1998;Garner et al, 2003;Wang et al, 2006]. Figure 8 shows n i for the four models.…”

Section: Sorting By Imf Directionmentioning

confidence: 99%

Ion heat flux and energy transport near the magnetotail neutral sheet

Kaufmann

Paterson

2008

J. Geophys. Res.

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“…Including this effect in (28) - (30) exacerbates the earthward decreases of p and n. At any rate, the above solution is a demonstration that the heat flux terms do lead to significant sub-adiabaticity, but are not purported to be realistic representations of the true magnetosphere, which must be solved in two dimensions and with (25) incorporated. Comparisons with empirical studies such as those by Wing and Newell [1998] and Wang et al [2006] need to be carried out. We will deal with this rather extensive problem in a separate study.…”

Section: Subadiabaticity In the Midnight Sectormentioning

confidence: 99%

Heat flux in magnetospheric convection: A calculation based on adiabatic drift theory

Liu

2006

Geophysical Research Letters

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[1] Empiric evidence and theoretical argument indicate that magnetospheric convection is globally sub-adiabatic. Reconciliation of the sub-adiabaticity with the underlying adiabatic particle drifts is a problem that has not been conclusively demonstrated. In this paper, through an ensemble average, we show that the Rice Convection Model contains a heat flux due to thermal inequilibrium between two adjacent flux tubes of equal volume. The averaged theory is based on field variables obeying a set of partial differential equations (Eulerian formulation), instead of conservative variables advecting with fluid elements (Langrangian formulation). We apply the theory to investigate a one-dimensional case of subadiabatic variation of thermodynamic properties in the plasma sheet.

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“…The energy stored for the triggering of the X lines and the substorm in the tail under northward IMF is just the remnant energy in the period of preexiting southward IMF [Li et al, 2008;Du et al, 2011;Miyashita et al, 2011]. Due to the weaker convection electric field for northward than southward IMF [Maezawa, 1976;Usadi et al, 1993;Borovsky et al, 1998;Petrukovich et al, 2003;Wang et al, 2006], it is prone to conjecture that not enough energy and/or magnetic flux can be deposited in the tail to form a thin current sheet and generate an X line under northward IMF condition [Min et al, 1985;Ma et al, 1995;Pritchett and Coroniti, 1994;Petrukovich et al, 2011].…”

Section: Introductionmentioning

confidence: 99%

X lines in the magnetotail for southward and northward IMF conditions

et al. 2015

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Utilizing associated observations of Geotail and ACE satellites from the year of 1998 to 2005, we investigated the X lines in the near‐Earth tail under different interplanetary magnetic field (IMF) conditions. The X lines are recognized by the tailward fast flows with negative Bz. Statistically, the X lines in the tail can be observed for southward as well as northward IMF, but more frequently observed for southward IMF. A typical case on 26 April 2005 showed clear evidence that the X line can occur for northward IMF while the geomagnetic activity is particularly quiet. Further analysis showed that the X line‐related solar wind has stronger Ey and Bz components for southward than northward IMF. In addition, the X line‐related geomagnetic activities are stronger for southward than northward IMF.

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Equatorial distributions of the plasma sheet ions, their electric and magnetic drifts, and magnetic fields under different interplanetary magnetic field B_z conditions

Cited by 83 publications

References 25 publications

Ion heat flux and energy transport near the magnetotail neutral sheet

Ion heat flux and energy transport near the magnetotail neutral sheet

Heat flux in magnetospheric convection: A calculation based on adiabatic drift theory

X lines in the magnetotail for southward and northward IMF conditions

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