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arXiv · 2506.00931

Population Synthesis Study on the Binary Origin of Type Ibn Supernovae

Takatoshi Ko·Tomoya Kinugawa·Daichi Tsuna·Ryosuke Hirai·Yuki Takei
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Abstract

Type Ibn supernovae (SNe) are a class of SN explosions whose progenitors are surrounded by dense helium-rich circumstellar matter (CSM). Some models have been proposed for how to form the dense CSM, with promising scenarios involving either binaries with a low-mass ($\lesssim 3~M_\odot$) helium (He) star, or mergers following common envelope phases between a He star and a compact object. Using rapid binary population synthesis calculations, we estimate the event rate of these channels and compare it with the observed SN Ibn rate. We find that exploding low-mass He stars in close binaries (of separations $\lesssim$ a few 100 $R_\odot$) can be sufficiently produced to account for the observed event rate of SN Ibn, while the merger scenario can likely account for only a fraction of these SNe. We discuss the types of companions expected in the low-mass He star scenario, finding massive main sequence stars ($10$--$20\ M_\odot$) to be typical, with a potentially non-negligible fraction ($<10\%$) of binaries with white dwarf (WD) companions that have long delay times of up to $100$ Myrs.

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Takatoshi Ko, Tomoya Kinugawa, Daichi Tsuna, Ryosuke Hirai, Yuki Takei. 2025-06-01. Population Synthesis Study on the Binary Origin of Type Ibn Supernovae. https://doi.org/10.1093/mnras%2Fstaf1241

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