- High-latitudedaysideenergeticprecipitationandIMF B rotations

The HILDCAA phase of the storm is characterized by fluctuations in the solar wind magnetic field B z component simultaneous with continuous high AE activity through the recovery

Average Magnetic field and Polar current System (AMPS) model values of Birkeland currents during purely northward interplanetary magnetic field for three different values of the

In addition, an in situ package will measure the composition and speed of the solar wind and the strength and orientation of interplanetary magnetic field, measurements crucial

(a) Snapshot of open (solid, dashed, dotted) field lines and one reconnected closed (thick) field line under the influence of the magnetic tension force (thick grey arrows) from IMF B

Here we extend an earlier study of the proton aurora in the cusp during northward interplanetary magnetic field (IMF) conditions [Frey et al., 2002] to southward IMF conditions..

The closed field lines on the dayside get twisted by the combination of erosion of flux at high-latitude flanks and by the increase of magnetic pressure in the northern dawn and

(b) A paramagnetic material will orient its internal magnetic moments along the external magnetic field, whereas a diamagnetic material will create a magnetic moment in the

Under a northward IMF condition, magnetic reconnection is limited to a small high latitude region and K–H instability becomes important in bringing solar wind energy and plasma into