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Simulations, Data Analysis and Algorithms

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Figure 3 | Computational Astrophysics and Cosmology

Figure 3

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

Figure 3

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 \(4.5 R_{\odot }\).

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