The separate contributions to the T96_01 model fields by the different solar wind dynamic inputs are plotted in Figure 4. Figure 4a shows the model field contributions due to the ring current while Figure 4b is plotted with a smaller vertical scale to emphasize the model field contributions from the solar wind dynamic pressure (dotted line) and the interplanetary magnetic field (solid line). These figures allow us to examine which solar wind inputs to the T96_01 model contribute the most to the model external magnetic fields. Given the good agreement between the T96_01 model and the POLAR MFE fields the assumption is made that the solar wind parameters also contribute to the observed magnetic field residuals in a similar manner.
© 1998 AGU