The Observer’s Guide to the Gamma-Ray Burst Supernova Connection

Figure 16

The effect of different degrees of nickel mixing in the ejecta of SNe Ibc on their observed LCs, from [290]. Top and middle panels: how the relative positions of the shock-heating contribution (blue curves), Ni diffusive tail contribution (purple curves), and the contribution (red curves) to the observed LC can differ depending on the depth and amount of mixing of the . The total observed LC is the sum of these three components. When the is located deep in the ejecta (middle panel) and the shock-heating light curve (blue curve) is below the detection limits, there can be a significant dark phase between the time of explosion and the moment of first detection. Bottom: temporal evolution of the photospheric radius (orange curve) and velocity (green curve). Depending on the position of the LC, different photospheric radii, velocities, and velocity gradients will be present during the rising LC.