吸积致塌缩型超新星前身星研究

吸积致塌缩型超新星在天体物理研究中占有非常重要的意义，在观测上有许多间接证据支持这类天体的存在，但其前身星仍没得到很好的研究。本项目将对这类超新星的前身星进行系统性研究，具体研究内容如下：给出各种白矮星吸积模型对这类超新星的贡献，将包含ONe WD+MS渠道、ONe WD+RG渠道、ONe WD+He star渠道及CO WD+He star渠道；给出各种双白矮星并合模型对这类超新星的贡献，将包含ONe WD+ONe WD渠道、ONe WD+CO WD渠道及CO WD+CO WD渠道；给出这些前身星模型诞生吸积致塌缩型超新星的初始参数空间、诞生率及延迟时标分布等，推测观测上的哪些大质量白矮星双星系统是吸积致塌缩型超新星的前身星候选体，并为吸积致塌缩型超新星爆发的数值模拟提供初始输入。通过本项目，将进一步加深人们对吸积致塌缩型超新星前身星本质的认识，并促进相关领域的发展。

Accretion-induced collapse (AIC) events play an important role in astrophysics. Many indirect evidence in the observations supports the existence of this type of objects, but the exact nature of their progenitors is still not well studied. In this project, we will study the progenitors of AIC events systematically, as follows. We will study various of white dwarf (WD) accretion model of AIC events, including the contributions of the ONe WD+MS channel, the ONe WD+RG channel, the ONe WD+He star channel and the CO WD+He star channel. We will study various of double WD merger model of AIC events, including the contributions of the ONe WD+ONe WD channel, the ONe WD+CO WD channel and the CO WD+CO WD channel. We will give the initial parameter space, birthrates and delay times of AIC events through these progenitor models, and speculate whether these observational massive WDs in the binaries will produce AIC events or not in the future. We will also provide initial parameter input for the explosion models of AIC events. This project will have important influences on the question of the progenitors of AIC events, and promote the development of related fields.