An explicit IMF By dependence on solar wind ‐ magnetosphere coupling

An explanation for the trend seen in Figure 5.6, with higher level of pressure piling for lean and rich mixtures, can be sought in the burning velocity’s dependence on

A superposed epoch analysis of the plasma sheet flows is presented in Figure 5, with the same format as Figure 1, though extended up to 4 hr after an IMF B y reversal. Since the

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

Now see the process from the inertial system of the space ship. In this system the light travels a perpendicular distance which is the same, 12 light years. The direction of 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

Within the polar cap, open magnetic field lines are tilted antisunwards by the flow of the solar wind, whereas in the return flow region field lines are tilted sunwards due to

This paper discusses counterstreaming electrons, electric field turbulence, HF radar spectral width enhancements, and field-aligned currents in the southward IMF cusp

The presence of fast and/or slow solar wind, an associated solar wind density enhancement and potential shock, and the duration and orientation of a magnetic cloud, all combine