Interacting Binary Stars as Progenitors for Interacting Supernovae

Le résumé fourni par la source

Abstract Dense, compact circumstellar media (CSM) are required to power strongly interacting supernovae (SNe), yet their physical origin remains uncertain. We present a systematic study of binary stellar evolution models computed with MESA , demonstrating that Case C mass transfer—initiated after core helium ignition—naturally produces the dense, nearby CSM inferred in interacting events. Across a grid of binary models, we find that donors of 10–20 M ⊙ in binaries with separations of ∼1000–2700 R ⊙ undergo late-stage Roche-lobe overflow within ∼10 3 yr prior to core collapse, ejecting ∼0.01–0.2 M ⊙ and forming CSM extending to ∼10 16 –10 18 cm. Our results suggest that the Case C mass transfer may account for ∼13% of all core-collapse supernova (SN) progenitors, rather than representing a rare channel. A subset of these Case C binaries produces CSM properties that are quantitatively in agreement with those inferred for interacting SNe such as SN 2014C. In contrast to earlier binary interactions or single-star mass loss, Case C transfer operates at the right time and scale to shape the immediate pre-SN environment without requiring ad hoc eruptive mechanisms. Our results identify late-stage binary interaction as a robust and physically motivated channel for producing the dense CSM that powers interacting SNe.

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