A grid of rotating PPISN progenitor models shows that faster rotation reduces ejected mass and shell energy while producing H-poor, C/O-rich shells, and one modeled shell collision gives a Type Ib/c-like transient.
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Rotational Dynamics in Pulsational Pair-Instability Supernovae: Implications for Mass-Loss and Transient Events
A grid of rotating PPISN progenitor models shows that faster rotation reduces ejected mass and shell energy while producing H-poor, C/O-rich shells, and one modeled shell collision gives a Type Ib/c-like transient.