Statistics of plasma sheet convection

Details Statistics of plasma sheet convection Statistics of plasma sheet convection

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011jgra..11608201j&link_type=abstract

Journal of Geophysical Research, Volume 116, Issue A8, CiteID A08201

Physics

1

Magnetospheric Physics: Plasma Convection (2463), Magnetospheric Physics: Plasma Sheet, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions

Scientific paper

Determining the characteristics of plasma sheet convection and their response to changes in various solar wind parameters is important for understanding the energy and mass transport, as well as disturbance propagation, through geospace. We use 15 years of data obtained by Geotail, Cluster, and THEMIS to study statistically the characteristics of plasma sheet flows and the effect of the interplanetary magnetic field (IMF) on the convection. We find that plasma sheet convection is dominated by slow speed (<100 km/s) flows that circulate around Earth on both sides toward the dayside. With increasing flow speed the sunward component of the flow velocity becomes more pronounced such that flows with V > 500 km/s are directed almost purely sunward. Both IMF By and IMF Bz are observed to penetrate the plasma sheet. During southward IMF conditions, a channel of increased Bz is created in the nightside around the aberrated midnight axis. We suggest that the channel is caused by dipolarization and magnetic flux pileup related to fast flows. The nightside region of highest mean flow speed is located more duskward during dawnward IMF conditions than during duskward IMF conditions. For plasma sheet flows with speeds higher than 100 km/s, we find that the orientation of IMF (clock angle) controls the speeds, while the magnitude of the solar wind electric field plays a minor role. The increasing speed indicates that energy transfer per unit length of the nightside X line increases as IMF turns southward.

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