Progenitors of Type IIb Supernovae. II. Observable Properties
Progenitors of Type IIb Supernovae. II. Observable Properties
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DOI：
10.3847/1538-4357/abb8d5
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发表时间：
2020-09
期刊：
影响因子：
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通讯作者：
N. Sravan;P. Marchant;V. Kalogera;D. Milisavljevic;R. Margutti
中科院分区：
文献类型：
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作者：
N. Sravan;P. Marchant;V. Kalogera;D. Milisavljevic;R. Margutti
IIb型超新星(SNE IIb)提供了一个独特的机会来研究由于各种观测限制而支配剥离包络SN前体演化的演化通道和机制。将这些限制条件与理论属性的完全分布进行比较，不仅有助于确定自然界中已观察到的属性的流行程度，而且还可以揭示当前未观察到的人口。在这篇后续论文中，我们使用了Sravan等人提出的大网格模型。得出单星和双星SNE IIb前驱性质的分布，并将它们与三个独立观测探测器的约束进行比较：多波段SN光曲线、直接前驱探测和X射线/射电观测。与之前的工作一致，我们发现虽然目前的观测排除了单星作为SN IIb前体，但双星中的SN IIb前体可以解释它们。我们还发现，这些分布表明在低金属丰度下存在一个未被观测到的双星SNE IIb的主要布居，这种布居是由于在Hertzsprung带隙上引发的质量转移引起的。特别是，我们的模型表明，存在一群高度剥离的(包络质量∼0.1M-0.2M☉)前体，它们是致密的(<；50R☉)和蓝色(Tef≲105K)，具有∼104.5-105.5 L☉和低密度星周介质。如Sravan等人所讨论的，这一组是解释SnIIb组分所必需的，并且可能存在，与金属丰度无关。我们的模型所指示的未观测到的群体的探测将支持微弱的恒星风和SN IIb前驱物质的低效质量转移。
Type IIb supernovae (SNe IIb) present a unique opportunity for investigating the evolutionary channels and mechanisms governing the evolution of stripped-envelope SN progenitors due to a variety of observational constraints. Comparison of these constraints with the full distribution of theoretical properties not only helps determine the prevalence of observed properties in nature, but can also reveal currently unobserved populations. In this follow-up paper, we use the large grid of models presented in Sravan et al. to derive distributions of single and binary SNe IIb progenitor properties and compare them to constraints from three independent observational probes: multiband SN light curves, direct progenitor detections, and X-ray/radio observations. Consistent with previous work, we find that while current observations exclude single stars as SN IIb progenitors, SN IIb progenitors in binaries can account for them. We also find that the distributions indicate the existence of an unobserved dominant population of binary SNe IIb at low metallicity that arise due to mass transfer initiated on the Hertzsprung Gap. In particular, our models indicate the existence of a group of highly stripped (envelope mass ∼0.1–0.2M☉) progenitors that are compact (<50R☉) and blue (Teff ≲ 105 K) with ∼104.5–105.5 L☉ and low-density circumstellar mediums. As discussed in Sravan et al., this group is necessary to account for SN IIb fractions and likely exist regardless of metallicity. The detection of the unobserved populations indicated by our models would support weak stellar winds and inefficient mass transfer in SN IIb progenitors.