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Supernova-driven turbulence can have massive effects on the evolution of the surrounding interstellar medium (ISM), affecting nearby star formation and the initial mass function. This makes supernovae an integral element to simulating the evolution of the ISM. Many previous supernova implementations make assumptions about the internal structure, size, or energy distribution of the supernovae that may not agree with accepted literature. In this talk, I present my implementation of supernovae based on the analytical Sedov solution, a self-similar blast wave solution linked to the main stage of supernova evolution. I apply this solution to exploring supernova-driven turbulence, finding the generated density and velocity power spectra to have scaling laws that are in line with current literature. |
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