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Simulations, Data Analysis and Algorithms

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Figure 15 | Computational Astrophysics and Cosmology

Figure 15

From: Simulations of stripped core-collapse supernovae in close binaries

Figure 15

Distribution of NS kick angles from the x -axis (aligned with the pre-kick NS orbital vector) for the same parameters as the Monte Carlo runs shown in Figure  14 (but with \(\pmb{2 \times10^{5}}\) samples to better fill the space in angles). The span of θ over \(\phi= 0\) defines the orbital plane, where \(\theta= 0\) is for a kick aligned with the NS orbital velocity vector. Panel (a) shows the case of no impact effects on the companion (blue distribution in Figure 14) and panel (b) shows the case where impact effects determined from our simulations are included (red distribution in Figure 14). Colours represent the magnitude of the companion star from disrupted binaries (as a fraction of the maximum runaway velocity). Grey shows cases where the NS and companion star merge. The white regions for large θ are cases where the binary remains bound and so there is no runaway companion.

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