AI 中文总结
本研究利用BPASS模型探究SEISNe的前身星与CSM，发现仅双星周盘场景可复现观测到的SEISNe特征，明确了相关前身星的质量与金属丰度范围，并指出需特定射电观测来约束双星周盘性质。
AI 中文摘要
研究剥离包层相互作用超新星（SEISNe）的前身星，对探索大质量恒星演化的最终阶段至关重要。然而，这类超新星十分罕见，其前身星的性质仍知之甚少。我们利用双星种群与光谱合成（BPASS）恒星演化模型，对SEISNe的前身星展开研究。30153个产生贫氢核心坍缩超新星（SN）的恒星模型涵盖了单星与双星，包含13种金属丰度（Z=10⁻⁵至0.04）。我们通过三种星周物质（CSM）场景，结合线驱动质量损失与洛希瓣溢流（RLOF）质量损失，重建了恒星最后10万年的CSM形成过程：一种场景仅考虑CSM的星风分布，另外两种场景涉及双星周盘（CBD）的形成。我们采用解析模型与基准SN爆炸参数，计算了每种场景的光变曲线参数。研究发现，仅两种CBD场景（无单星模型）能复现观测到的SEISNe的光度与上升时间，其推导出的发生率与观测结果相当。预期的前身星仅在以下模型中被发现：零龄主序（ZAMS）质量为14-40倍太阳质量（M☉）且金属丰度≥太阳金属丰度（Z☉），以及ZAMS质量为30-40M☉且金属丰度<Z☉的模型。射电辐射建模表明，需开展早期（≤8天）、高频（≥70GHz）的观测，才能限制这类系统中CBD的性质。这些结果显示，若不存在爆发性质量损失等现象，SEISNe需要大质量恒星处于双星系统中，才能产生足够质量的CSM并将其限制在前身星附近。
英文摘要
Understanding the progenitors of stripped-envelope interacting supernovae (SEISNe) is crucial for probing the final stages of massive star evolution. Despite this, their rarity means the nature of their progenitors remains poorly constrained. We investigate the progenitors of SEISNe, using the Binary Population and Spectral Synthesis stellar evolution models. The 30,153 stellar models that result in hydrogen-poor core-collapse supernovae (SN) includes both binary and single stars, spanning 13 metallicities ($Z=10^{-5}$ to $0.04$). Circumstellar material (CSM) formation during their last 100\,kyr is reconstructed from line-driven and Roche lobe overflow (RLOF) mass loss using three scenarios for the CSM, one looking at a wind only distribution for the CSM, and two involving the formation of a circum-binary disc (CBD). Light curve parameters from each scenario are calculated using an analytical model and fiducial SN explosion parameters. We find only the two CBD scenarios, and consequently no single star models, reproduce the luminosities and rise times of observed SEISNe. The inferred rates are comparable to observations. Expected progenitors were only found in models with ZAMS masses of $14-40\,$M$_{\odot}$ at $\geq Z_\odot$ and $30-40\,$M$_{\odot}$ at $< Z_\odot$. Modelling the radio emissions shows that early ($\leq8\,$days) and high frequency ($\geq70\,$GHz) observations are required to constrain the nature of CBDs in these systems. These results indicate that, without phenomena such as eruptive mass loss, SEISNe require massive stars in binary systems in order to produce sufficient masses of CSM and confine them close to the progenitor.
Comments22 pages, 13 figures, accepted to MNRAS
