Figure 3
From: Simulations of stripped core-collapse supernovae in close binaries
Distribution of total energy in the gas, in units of foe ( \(\pmb{10^{51} \text{ ergs}}\) ), as a function of time following the supernova event. The energy is broken down into kinetic (\(E_{\mathrm{k}}\)), potential (\(E_{\mathrm{p}}\)) and internal (thermal) (\(E_{\mathrm{t}}\)). This example corresponds to a primary of mass \(4 M_{\odot }\) and an orbital separation of \(4.5 R_{\odot }\).