The accretion-induced collapse (AIC) scenario was proposed 40 years ago as an evolutionary end state of oxygen-neon white-dwarfs (ONe WDs), linking them to the formation of neutron star (NS) systems. However, there has been no direct detection of any AIC event so far, even though there exists a lot of indirect observational evidence. Meanwhile, the evolutionary pathways resulting in NS formation through AIC are still not well investigated. In this article, we review recent studies on the two classic progenitor models of AIC events, i.e., the single-degenerate model (including the ONe WD+MS/RG/He star channels and the CO WD+He star channel) and the double-degenerate model (including the double CO/ONe WD channels and the ONe WD+CO WD channel). Recent progress on these progenitor models is reviewed, including the evolutionary scenarios, the initial parameter space and the related objects. For the single-degenerate model, the pre-AIC systems could potentially be identified as supersoft X-ray sources, symbiotics and cataclysmic variables, whereas the post-AIC systems could be identified as low-/intermediate-mass X-ray binaries and the resulting low-/intermediate-mass binary pulsars, most notably millisecond pulsars. For the double-degenerate model, the pre-AIC systems are close double WDs, whereas the post-AIC systems are isolated NSs with peculiar properties. We also review the predicted rates of AIC events, the mass distribution of NSs, and the gravitational wave (GW) signals from double WDs that are potential GW sources in the Galaxy in the context of future space-based GW detectors. Recent theoretical and observational constraints on the detection of AIC events are summarized. In order to confirm the existence of the AIC process, and resolve this long-term issue presented by current stellar evolution theories, more numerical simulations and observational identifications are required.

中文翻译：

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白矮星双星吸积引起的坍缩形成中子星系统

吸积引起的坍缩 (AIC) 情景是 40 年前提出的，作为氧-氖白矮星 (ONE WD) 的演化终结状态，将它们与中子星 (NS) 系统的形成联系起来。然而，尽管存在大量间接观测证据，但迄今为止还没有直接检测到任何 AIC 事件。同时，通过 AIC 导致 NS 形成的进化途径仍未得到很好的研究。在本文中，我们回顾了最近对 AIC 事件的两个经典前身模型的研究，即单退化模型（包括 ONe WD+MS/RG/He 星通道和 CO WD+He 星通道）和双退化模型。 -退化模型（包括双CO/ONe WD通道和ONe WD+CO WD通道）。回顾了这些祖先模型的最新进展，包括进化场景，初始参数空间和相关对象。对于单简并模型，AIC 前系统可能被识别为超软 X 射线源、共生体和灾变变量，而 AIC 后系统可以被识别为低/中质量 X 射线双星和由此产生的低/中等质量双星脉冲星，最显着的是毫秒脉冲星。对于双退化模型，前 AIC 系统是接近的双 WD，而后 AIC 系统是具有特殊性质的孤立 NS。我们还回顾了 AIC 事件的预测速率、NS 的质量分布以及来自双 WD 的引力波 (GW) 信号，这些信号是未来天基 GW 探测器背景下银河系中潜在的 GW 源。总结了最近对 AIC 事件检测的理论和观察限制。