The influence of rotation and metallicity on the explodability of massive stars

Abstract

During the late stages of massive stellar evolution, failed supernovae (FSN) may form through core-collapse processes. The traditional evaluation criterion ${\xi }_{2.5}$ $=$ 0.45, primarily established using non-rotating progenitor models, suffers from significant inaccuracies when applied to rotating pre-supernova systems. The effects of metallicity and rotation on the explodability landscapes of massive stars lack robust quantification. We aim to investigate how rotation and metallicity influence the explodability of massive stars. We investigate how rotation and metallicity affect stellar explodability using MESA simulations with initial rotational velocities of $0$, $300$, and $600\mathrm{km},{\mathrm{s}}^{-1}$ at three metallicities ($Z_{\odot }$, $1/10,Z_{\odot }$, $1/50,Z_{\odot }$). Core-collapse phases are simulated with GR1D to determine critical heating efficiencies. Our results yield revised ${\xi }_{2.5}$ criteria: 0.45 for non-rotating models; 0.48 for $300\mathrm{km},{\mathrm{s}}^{-1}$; 0.47 for $600\mathrm{km},{\mathrm{s}}^{-1}$ at solar metallicity; and 0.59 for low-metallicity models. Chemically homogeneous evolution in rapidly rotating low-metallicity stars significantly raises the compactness limit for successful explosions and narrows the zero-age main sequence mass range for failed supernovae. Rotation substantially affects the explodability of low-metallicity massive stars, underscoring the importance of incorporating rotational effects in models of core-collapse supernova progenitors.

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