The driving of the plasma sheet by the solar wind

Borovsky, Joseph E.; Thomsen, M. F.; Elphic, R. C.

doi:10.1029/97ja02986

Cited by 341 publications

(432 citation statements)

References 126 publications

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“…From 3 two-satellite studies that the authors have performed involving simultaneous solar wind and plasma sheet data (ISEE-3 and ISEE 2, IMP-8 and 1989-046, and WIND and 1994-085), it has been found that the plasma sheet density is strongly correlated with the solar wind density and that the plasma sheet temperature is strongly correlated with the solar wind flow speed [Delapp et al, 1995;Borovsky et al, 1997bBorovsky et al, , 1998a. (Whereas the plasma sheet density is poorly correlated with the solar wind speed and the plasma sheet temperature is poorly correlated with the solar wind density.)…”

Section: Goertz and Baumjohann [1991] Predicted This Decreasementioning

confidence: 99%

The transport of plasma sheet material from the distant tail to geosynchronous orbit

Borovsky¹,

Thomsen²,

Elphic³

et al. 1998

J. Geophys. Res.

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131

166

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Abstract. Several aspects of mass transport in the Earth's plasma sheet are examined. The evolution of plasma sheet material as it moves earthward is examined by statistically comparing plasma sheet properties at three different downtail distances: nearEarth plasma sheet properties obtained from measurements by 1989-046 near the geomagnetic equator near midnight at 6.6 RE, midtail plasma sheet properties obtained from ISEE 2 measurements during 333 encounters with the neutral sheet, and distant-plasma sheet properties obtained from ISEE 2 measurements during 53 encounters with the interface between the plasma sheet and the plasma sheet boundary layer. Examination of the evolution of the plasma sheet through pressure-density space shows that the transport is nearly adiabatic (ff -1.52), with a loss of entropy observed in the near-Earth region. Th e estimated pressure loss from the plasma'sheet associated with the aurora is able to account for the observed decrease in entropy. The near-Earth plasma sheet plasma is also found to be compressed much less than would be expected from magnetic field models.

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Section: Goertz and Baumjohann [1991] Predicted This Decreasementioning

confidence: 99%

The transport of plasma sheet material from the distant tail to geosynchronous orbit

Borovsky¹,

Thomsen²,

Elphic³

et al. 1998

J. Geophys. Res.

Self Cite

131

166

View full text Add to dashboard Cite

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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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“…Extensive statistical studies of the plasma within the near-Earth magnetosphere have previously revealed the behaviour of such parameters (e.g. Baumjohann et al, 1988;Newell and Meng, 1992;Borovsky et al, 1998;Wing and Newell, 1998;Měrka et al, 2002;Tysganenko and Mukai, 2003;Wing et al, 2005;Neagu et al, 2005;Denton et al, 2005Denton et al, , 2006Borovsky and Denton, 2006a, b;Lavraud et al, 2005Lavraud et al, , 2006Thomsen et al, 2007;Nagata et al, 2007;Åsnes et al, 2008) under a variety of conditions. The primary aim of the work outlined in the current paper is to reveal the averaged bulk parameters in the magnetosphere as a first step to a determination of how such parameters evolve during geomagnetic disturbances.…”

Section: Introductionmentioning

confidence: 99%

Solar wind dependence of ion parameters in the Earth's magnetospheric region calculated from CLUSTER observations

Denton

Taylor

2008

Ann. Geophys.

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Abstract. Moments calculated from the ion distributions (∼0-40 keV) measured by the Cluster Ion Spectrometry (CIS) instrument are combined with data from the Cluster Flux Gate Magnetometer (FGM) instrument and used to characterise the bulk properties of the plasma in the nearEarth magnetosphere over five years (2001)(2002)(2003)(2004)(2005). Results are presented in the form of 2-D xy, xz and yz GSM cuts through the magnetosphere using data obtained from the Cluster Science Data System (CSDS) and the Cluster Active Archive (CAA). Analysis reveals the distribution of ∼0-40 keV ions in the inner magnetosphere is highly ordered and highly responsive to changes in solar wind velocity. Specifically, elevations in temperature are found to occur across the entire nightside plasma sheet region during times of fast solar wind. We demonstrate that the nightside plasma sheet ion temperature at a downtail distance of ∼12 to 19 Earth radii increases by a factor of ∼2 during periods of fast solar wind (500-1000 km s −1 ) compared to periods of slow solar wind (100-400 km s −1 ). The spatial extent of these increases are shown in the xy, xz and yz GSM planes. The results from the study have implications for modelling studies and simulations of solar-wind/magnetosphere coupling, which ultimately rely on in situ observations of the plasma sheet properties for input/boundary conditions.

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The driving of the plasma sheet by the solar wind

Cited by 341 publications

References 126 publications

The transport of plasma sheet material from the distant tail to geosynchronous orbit

The transport of plasma sheet material from the distant tail to geosynchronous orbit

X lines in the magnetotail for southward and northward IMF conditions

Solar wind dependence of ion parameters in the Earth's magnetospheric region calculated from CLUSTER observations

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