Ia型超新星在行星状星云内爆炸的比例
The fraction of type Ia supernovae exploding inside planetary nebulae (SNIPs)
摘要：
使用三个独立的方向，我们估计Ia型超新星（SNe Ia）在行星状星云（PNe）内爆炸的比例至少为20%。我们的三个方向如下。(i)最近有人声称，一些Ia超新星中的钠吸收线是源于大质量的星周物质（CSM），我们使用Sternberg等人（2014）的结果来暗示，> ~20%的Ia超新星发生在PN（或PN后代）内部，因此将它们归类为SNIP。(ii)我们接下来使用的结果表明，只要在Ia超新星中有氢线，CSM中的氢质量就很大（> 1 M_Sun），因此爆炸是SNIP。我们做了一个最简单的假设，即在核心简并的框架下，在核心与白矮星（WD）合并后的10^5年内，爆炸的概率在时间上是恒定的。这导致至少几个x10的SNe Ia可能具有SNIP起源。(iii)我们研究了13个分辨率良好的近距离超新星遗迹（SNRs）Ia的X射线形态，并得出一个粗略的上限，根据该上限，10-30%的所有SNRs Ia具有相反的耳状特征，我们将其作为SNIP起源的证据。我们的研究结果，连同其他几个最近的结果，使我们得出结论，两个方案最有助于Ia超新星的核心简并和双简并的情况。这两个加起来占所有SNe Ia的>95%。
英文摘要：
Using three independent directions we estimate that the fraction of type Ia supernovae (SNe Ia) exploding inside planetary nebulae (PNe), termed SNIPs,is at least ~20%. Our three directions are as follows. (i) Taking the variable sodium absorption lines in some SN Ia to originate in a massive circumstellar matter (CSM), as has been claimed recently, we use the results of Sternberg et al. (2014) to imply that > ~20% of SN Ia occur inside a PN (or a PN descendant), hence classify them as SNIPs. (ii) We next use results that show that whenever there are hydrogen lines in SN Ia the hydrogen mass in the CSM is large (> 1 M_Sun), hence the explosion is a SNIP. We make the simplest assumption that the probability for explosion is constant in time for up to about 10^5 yrs after the merger of the core with the white dwarf (WD) in the frame of the core-degenerate scenario. This results with at least few x10 of SNe Ia that may have a SNIP origin. (iii) We examine the X-ray morphologies of 13 well-resolved close-by SN remnants (SNRs) Ia and derive a crude upper limit, according to which 10-30% of all SNRs Ia possess opposite ear-like features, which we take as evidence of SNIP origin. Our results, together with several other recent results, lead us to conclude that the two scenarios most contributing to SNe Ia are the core degenerate and the double degenerate scenarios. Together these two account for >95% of all SNe Ia.
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