Heliosphere¶

2D slice animations of the heliospheric MHD solution. Each row shows one quantity for equatorial and meridional cuts. For time-dependent runs the MHD solution evolves each frame, while for steady-state runs the background is fixed and spacecraft positions change through it. Density and radial field are scaled by \(r^2\) to remove the geometric \(1/r^2\) falloff, revealing intrinsic structure in the solar wind.