Figure 10
From: Simulations of stripped core-collapse supernovae in close binaries
Blue lines show the profiles of (a)Â density, (b)Â magnitude of velocity and (c)Â the mass distribution of velocity within the ejecta for our simulations (binned in radial shells form the centre of mass of the ejecta). Black dashed lines show the power-law profiles used in Liu et al. (2015). Both cases were calculated for a time of 90Â s after the supernova. The transition velocity (and radius at which this occurs) in the Liu et al. (2015) profiles are given as dotted lines.