English: Streamlines of charged particles from a plasma wind (e.g., from the Sun or a Star) flow from left to right at velocity w. A source attached to a spacecraft generates a magnetic field. At the boundary where magnetic pressure equals plasma wind kinetic pressure an artificial magnetopause forms at a characteristic Length L (m) from the field source, which compresses the magnetic field lines facing the oncoming plasma wind. The magnetopause deflects charged particles, which affects their streamlines and increases the density at magnetopause. A magnetospheric bubble or cavity forms that has very low density downstream from the magnetopause. At the boundary where pressure of the plasma wind equals the magnetic pressure a magnetopause forms, upstream from which a bow shock develops. Simulation results often show the particle density through use of color with an example shown in the figure according to the legend in the lower left.