Abstrakt
We investigate the magnetopause (MP) location influenced by large solar wind (SW) structures: magnetic clouds (MCs), interplanetary coronal mass ejections (ICMEs), and intervals following interplanetary shocks (IPs) driven by these structures and compare it with the MP location in the pristine SW. We focus on the differences between predicted and encountered MP locations near the subsolar point.
For predictions, we used the MP model of Shue et al. [1997] where Wind plasma and magnetic field parameters from 2007 to 2015 have been applied as input data. Into the model, we added other pressure components reflecting the different alpha particle content and larger magnetic field.
We found that differences between the modeled and observed (by the THEMIS spacecraft) MP locations in the subsolar region are small but systematic. We discuss changes in model predictions and other factors which are not included in the model but can affect of the magnetopause location (for example, geomagnetic activity demonstrated by SYM-H and AE indices in our case).