论文标题
仔细观察他的明星，作为生产IA型超新星型旧种群的渠道
A closer look at non-interacting He stars as a channel for producing the old population of Type Ia supernovae
论文作者
论文摘要
IA型超新星（SNE IA）祖细胞的性质仍然是一个谜。由白矮人（WD）组成的二进制系统和主要序列（MS）供体是SNE IA的潜在祖细胞，其中，当其质量达到同伴恒星材料增值期间，其质量达到Chandrasekhar极限时，可能会发生WD的热核爆炸。在目前的工作中，我们解决了特定的MS供体通道的理论速率和延迟时间，其中She+MS二进制于公共包膜事件产生的二元二进制于随后形成WD+MS系统，而没有Roche Lobe Lobe溢出质量的He Star。通过将自洽的二进制进化计算的结果与人口合成模型相结合，我们发现该渠道中SNE IA的贡献约为每年2.0e-4。此外，我们发现该通道中SNE IA的延迟时间覆盖约1.0-2.6 GYR的范围，几乎所有以这种方式生成的SNE IA（约97％）的延迟时间> 1> 1 GYR。尽管这项工作的SN IA速率约为总SN IA率的10％，但该渠道代表了对观察到的SNE IA的旧人群（1-3 GYR）的可能贡献。
The nature of the progenitors of type Ia supernovae (SNe Ia) remains a mystery. Binary systems consisting of a white dwarf (WD) and a main-sequence (MS) donor are potential progenitors of SNe Ia, in which a thermonuclear explosion of the WD may occur when its mass reaches the Chandrasekhar limit during accretion of material from a companion star. In the present work, we address theoretical rates and delay times of a specific MS donor channel to SNe Ia, in which a He star+MS binary produced from a common envelope event subsequently forms a WD+MS system without the He star undergoing mass transfer by Roche lobe overflow. By combining the results of self-consistent binary evolution calculations with population synthesis models, we find that the contribution of SNe Ia in this channel is around 2.0e-4 per year. In addition, we find that delay times of SNe Ia in this channel cover a range of about 1.0-2.6 Gyr, and almost all SNe Ia produced in this way (about 97%) have a delay time of > 1 Gyr. While the rate of SN Ia in this work is about 10% of the overall SN Ia rate, the channel represents a possible contribution to the old population (1-3 Gyr) of observed SNe Ia.
