Open AccessGeomagnetic signatures of current wedge produced by fast flows in a plasma sheet
Author(s) -
Cao JinBin,
Yan Chunxiao,
Dunlop Malcolm,
Reme Henri,
Dandouras Iannis,
Zhang Tielong,
Yang Dongmei,
Moiseyev Alexey,
Solovyev Stepan I.,
Wang Z. Q.,
Leonoviche A.,
Zolotukhi.,
Mishin V.
Publication year - 2010
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/2009ja014891
Subject(s) - substorm , earth's magnetic field , electrojet , geophysics , middle latitudes , solar wind , ionosphere , plasma sheet , geology , current (fluid) , physics , geomagnetic storm , interplanetary magnetic field , plasma , magnetic field , atmospheric sciences , magnetosphere , oceanography , quantum mechanics
This paper uses the plasma data from Cluster and TC‐1 and geomagnetic data to study the geomagnetic signatures of the current wedge produced by fast‐flow braking in the plasma sheet. The three fast flows studied here occurred in a very quiet background and were accompanied by no (or weak) particle injections, thus avoiding the influences from other disturbances. All the geomagnetic signatures of a substorm current wedge can be found in the geomagnetic signatures of a current system produced by the braking of fast flows, indicating that the fast flows can produce a complete current wedge which contains postmidnight downward and premidnight upward field‐aligned currents, as well as a westward electrojet. The Pi2 precursors exist not only at high latitudes but also at midlatitudes. The starting times of midlatitude Pi2 precursors can be identified more precisely than those of high‐latitude Pi2 precursors, providing a possible method to determine the starting time of fast flows in their source regions. The AL drop that a bursty bulk flow produces is proportional to its velocity and duration. In three cases, the AL drops are <100 nT. Because the AE increase of a typical substorm is >200 nT, whether a substorm can be triggered depends mainly on the conditions of the braking regions before fast flows. The observations of solar wind before the three fast flows suggest that it is difficult for the fast flows to trigger a substorm when the interplanetary magnetic field B z of solar wind is weakly southward.