The three-dimensional structure of the disk–corona inner region as seen from 30° above the equator (similar to Figure 1, left panels). The left panel shows a white isosurface of n = 10¹⁰ cm⁻³, which represents the higher-density region of the disk. The two initial gaps in the isosurface are due to the tilt of the stellar dipole field. The blue lines mark selected magnetic field lines that cover the displayed region. The middle panel shows the same isosurface with red-colored velocity streamlines. In the right panel, we show the equatorial plane colored with contours of the temperature, where blue regions mark the cold disk material and red regions mark the hot corona. These are sample snapshots for t = 0 (top panels) and t = 108 hr (bottom panels). An animation of this figure is available. The animation starts at t = 0 and ends at t = 108:30 hr in 30 minute steps. The real-time duration of the animation is 37 s, and it covers the full 108.5 hr of the simulation. 

(An animation of this figure is available.)

The video/animation of this figure is available in the online journal.