Solar-wind control of plasma sheet dynamics

Abstract

Abstract. The purpose of this study is to quantify how solarwind conditions affect the energy and plasma transport in the geomagnetic tail and its large-scale configuration. To identify the role of various effects, the magnetospheric data were sorted according to different solar-wind plasma and interplanetary magnetic field (IMF) parameters: speed, dynamic pressure, IMF north-south component, epsilon parameter, Auroral Electrojet (AE) index and IMF ultra low-frequency (ULF) fluctuation power. We study variations in the average flow speed pattern and the occurrence rate of fast flow bursts in the magnetotail during different solar-wind conditions using magnetospheric data from five Time History of Events and Macroscale Interactions during Substorms (THEMIS) mission spacecraft and solar-wind data from NASA's OMNIWeb. The time interval covers the years from 2008 to 2011 during the deep solar minimum between cycles 23 and 24 and the relatively quiet rising phase of cycle 24. Hence, we investigate magnetospheric processes and solar-windmagnetospheric coupling during a relatively quiet state of the magnetosphere. We show that the occurrence rate of the fast (|V tail | > 100 km s −1 ) sunward flows varies under different solar-wind conditions more than the occurrence of the fast tailward flows. The occurrence frequency of the fast tailward flows does not change much with the solar-wind conditions. We also note that the sign of the IMF B Z has the most visible effect on the occurrence rate and pattern of the fast sunward flows. High-speed flow bursts are more common during the slow than fast solar-wind conditions.

Fast plasma sheet flows and X line motion in the Earth's magnetotail: results from a global hybrid-Vlasov simulation

“…Regions of piled-up magnetic flux are observed in front of BBFs. The sharp (a few seconds) increase in the z component of the magnetic field (B z ) at the leading edge of the piled-up flux is called the dipolarization front (Angelopoulos et al, 1992;Nakamura et al, 2011;Runov et al, 2009). The sharp increase (on the order of 10 nT) is typically preceded by a small (on the order of a few nT) transient decrease in B z , reaching in some cases negative values (Ohtani et al, 1992(Ohtani et al, , 2004.…”