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Possible explosive paths
View Larger Version | Depending on the model and the details that researchers incorporate, a supernova’s transition from the slow-burn phase, deflagration, to the fast-burn phase, detonation, can produce different amounts of nickel-56, leading to different inherent brightnesses for the exploded star. Credit: V. Gamezo, A. Khokhlov, E. Oran, Astrophysical Journal 2005

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