Detached and continuous circumstellar matter in Type Ibc supernovae from mass eruption
- Creators
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Tsuna, Daichi
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Takei, Yuki
Abstract
Some hydrogen-poor supernovae (SNe) are found to undergo interaction with dense circumstellar matter (CSM) that may originate from mass eruption(s) just prior to core-collapse. We model the interaction between the remaining star and the bound part of the erupted CSM that eventually falls back to the star. We find that while fallback initially results in a continuous CSM down to the star, feedback processes from the star can push the CSM to large radii of ≳10¹⁵ cm for several years after the eruption. In the latter case, a tenuous bubble surrounded by a dense and detached CSM extending to ≳10¹⁶ cm is expected. Our model offers a natural unifying explanation for the diverse CSM structures seen in hydrogen-poor SNe, such as Type Ibn/Icn SNe that show CSM signatures soon after explosion, and the recently discovered Type Ic SNe 2021ocs and 2022xxf (the "Bactrian") with CSM signatures seen only at late times.
Additional Information
© The Author(s) 2023. Published by Oxford University Press on behalf of the Astronomical Society of Japan. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). DT thanks Jim Fuller, Toshikazu Shigeyama, and Akihiro Suzuki for discussions, and the anonymous referee for constructive comments. DT is supported by the Sherman Fairchild Postdoctoral Fellowship at Caltech.Additional details
- Eprint ID
- 122355
- Resolver ID
- CaltechAUTHORS:20230719-853110800.4
- Sherman Fairchild Foundation
- Created
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2023-07-25Created from EPrint's datestamp field
- Updated
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2023-07-25Created from EPrint's last_modified field
- Caltech groups
- TAPIR, Walter Burke Institute for Theoretical Physics