亚发光和过发光Ia型超新星的诞生率
The birth rate of subluminous and overluminous type Ia supernovae
摘要：
基于Chen & Li（2009）和Pakmor et al.（2010）的结果，我们进行了一系列的二进制布居合成计算，并考虑了两种处理公共包络（CE）演化的方法，即$α$ -形式主义和$γ$ -算法.我们发现，这些独特的SNe Ia的出生率的演变在很大程度上取决于如何对待CE的演变。过亮的超新星Ia只可能出现在CE喷射效率低的$α$形式中，超新星Ia的延迟时间在0.4和0.8 Gyr之间。超新星对所有Ia超新星贡献率的上限小于0.3%。对于$α$ --用$α=3.0$的形式主义，等质量DD系统的亚发光超新星Ia的延迟时间在0.1和0.3 Gyr之间，而对于$α=1.0$则大于9 Gyr。$γ$算法的延迟时间范围很宽，即长于0.22 Gyr，甚至长达15 Gyr。来自等质量DD系统的次亮Ia超新星可能只占所有观测到的Ia超新星的不到1%。Chen & Li（2009）提出的超Bracrasekhar质量模型可以解释部分2003年的类fg超新星事件，Pakmor等人（2010）提出的等质量DD模型也可以解释部分1991年的类bg事件。此外，通过对1991 bg类超新星事件的诞生率和延迟时间等理论和观测结果的比较，我们发现，如果等质量DD系统是1991 bg类超新星Ia的前身，那么$γ$算法比$α$算法更适合于DD系统的CE演化.
英文摘要：
Based on the results of Chen & Li (2009) and Pakmor et al. (2010), we carried out a series of binary population synthesis calculations and considered two treatment of common envelope (CE) evolution, i.e. $α$-formalism and $γ$-algorithm. We found that the evolution of birth rate of these peculiar SNe Ia is heavily dependent on how to treat the CE evolution. The over-luminous SNe Ia may only occur for $α$-formalism with low CE ejection efficiency and the delay time of the SNe Ia is between 0.4 and 0.8 Gyr. The upper limit of the contribution rate of the supernovae to all SN Ia is less than 0.3%. The delay time of sub-luminous SNe Ia from equal-mass DD systems is between 0.1 and 0.3 Gyr for $α$-formalism with $α=3.0$, while longer than 9 Gyr for $α=1.0$. The range of the delay time for $γ$-algorithm is very wide, i.e. longer than 0.22 Gyr, even as long as 15 Gyr. The sub-luminous SNe Ia from equal-mass DD systems may only account for no more than 1% of all SNe Ia observed. The super-Chandrasekhar mass model of Chen & Li (2009) may account for a part of 2003fg-like supernovae and the equal-mass DD model developed by Pakmor et al. (2010) may explain some 1991bg-like events, too. In addition, based on the comparison between theories and observations, including the birth rate and delay time of the 1991bg-like events, we found that the $γ$-algorithm is more likely to be an appropriate prescription of the CE evolution of DD systems than the $α$-formalism if the equal-mass DD systems is the progenitor of 1991bg-like SNe Ia.
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