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PURE MAGNETISM. “As the IMF turns southward, dayside reconnection changes the conditions at the magnetospheric boundaries and begins to increase the open flux content in the magnetotail. In order to maintain pressure balance between the plasma sheet plasma pressure and the lobe magnetic pressure, the cross-tail current intensifies and the plasma sheet is compressed.” (IMF= interplanetary magnetic field). https://link.springer.com/article/10.12942/lrsp-2007-1 View in LinkedIn

DYNAMIC ENERGY FLOW. “The reconnection process is associated with rapid and significant energy conversion from magnetic energy in the magnetotail lobes to particle kinetic energy and heat in the plasma sheet.” https://link.springer.com/article/10.12942/lrsp-2007-1 View in LinkedIn

FLUID PLASMA SHEETS. “As the flows created by magnetic reconnection in the tail enter the inner magnetosphere, the large-scale magnetic field configuration changes rapidly from highly taillike to a much more quasidipolar state.” https://link.springer.com/article/10.12942/lrsp-2007-1 View in LinkedIn

STORM EFFECTS. “During magnetospheric substorms, a thin and intense current sheet forms in the inner part of the magnetotail as a consequence of the intensified driving.” https://link.springer.com/article/10.12942/lrsp-2007-1 View in LinkedIn

LAYERED PLASMA SHEETS. “The thin current sheet is often in the ion gyroradius scale, and can host very high current densities at the field reversal region; Furthermore, complex, bifurcated current sheets and large-scale wavy structures have been identified from multi-spacecraft analyses.” https://link.springer.com/article/10.12942/lrsp-2007-1 View in LinkedIn

PLASMA SHEETS. “In the region tailward of geostationary orbit out to about 20–30 RE the changes in the current density are not uniform: the total current is distributed between the pre-existing thick plasma/current sheet and a newly formed thin current sheet embedded within the plasma sheet.” https://link.springer.com/article/10.12942/lrsp-2007-1 View in LinkedIn