Multimessengers from Core-Collapse Supernovae: Multidimensionality as a Key to Bridge Theory and Observation
Figure 18
Left and middle panels show magnetic pressure (red line) versus ram pressure (blue line) for a typical MHD model (same as Figure 17) along the polar axis (a) or the equatorial plane (b) at 2 ms after the revival of the stalled bounce shock. The matter pressure is shown by green line as a reference. The right panel shows a velocity profile along the pole measured from the shock-stall (0.0 ms in the panel). For the equator, the magnetic pressure is much less than the ram pressure (middle panel), while the magnetic pressure amplified by the field wrapping along the pole becomes as high as the ram pressure of the infalling material at the shock front ((a), note that the shock position can be inferred by the discontinuity at around 150 km), leading to the MHD-driven shock formation (c). These figures are taken from [216].
