Detached and Continuous Circumstellar Matter in Type Ibc Supernovae from Mass Eruption

TL;DR

This paper models the interaction between supernova progenitors and circumstellar matter resulting from pre-explosion mass eruptions, explaining diverse observed CSM structures in hydrogen-poor supernovae.

Contribution

It introduces a model of fallback and feedback processes that account for both continuous and detached CSM structures in Type Ibc supernovae.

Findings

Fallback leads to initial continuous CSM close to the star.

Feedback processes can push CSM to large radii over years.

The model explains diverse CSM signatures in hydrogen-poor SNe.

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 fall 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 $\gtrsim 10^{15}$ cm from several years after the eruption. In the latter case, a tenuous bubble surrounded by a dense and detached CSM extending to $\gtrsim 10^{16}$ 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.