Figure 7
From: Simulations of stripped core-collapse supernovae in close binaries
Final mass lost from the companion as a function of orbital separation. Circles show results with a primary star of \(\pmb{3 M_{\odot }}\) and squares show results for a primary star of \(\pmb{4 M_{\odot }}\) . The secondary is \(1 M_{\odot }\) in each case. The solid lines show the best fit power-laws for each ejecta mass. The comparison curves are from the theoretical predictions of WLK75 as adapted by TT98 and Tauris (2015) (rescaled to our initial conditions), as well as the simulation results of Liu et al. (2015) for a \(0.9 M_{\odot }\) companion star. Note that the comparison with Liu et al. (2015) is not fully equivalent, as both the ejecta mass and companion mass (and therefore radius) are slightly different.