Journal of Geophysical Research: Space Physics

In the bot- tom panel of Figure 11, which shows the time pro fi le of the Dst index, the colors of the vertical lines indicate the L-shells of EMIC wave activity during the

We want to compare how the speed of the nightside convection on closed field lines in the dawn and dusk convection cells varies for different IMF directions

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

Sorting the data according to the location of the sunlight terminator and orientation of the interplanetary magnetic field (IMF), we find that the equivalent current resembles

It is therefore necessary to model subauroral ionospheric convection during geomagnetically quiet conditions and to compare the results with longitudinally extended observations

Figure 2 shows a 20 ms window with reference time 25 October 2012 13:27:13.221 UT. The RHESSI counts are shown as blue dots with a logarithmic energy scale on the y axis. The

The simulation results show that increased initial density before the onset of precipitation leads to smaller electron temperature increases, longer ionospheric heating

The table shows the following, in columns from left to right: The date of each event, whether or not UVI is available, the IMF B y at onset, the dipole tilt