The Type II supernovae 2006V and 2006au: two SN 1987A-like events
The Type II supernovae 2006V and 2006au: two SN 1987A-like events
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II 型超新星 2006V 和 2006au：两个类似 SN 1987A 的事件
DOI：
10.1017/s1743921312013555
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
F. Taddia
中科院分区：
文献类型：
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作者：
F. Taddia
摘要我们研究了超新星(SNE)2006V和2006Au的光学和近红外(NIR)光曲线和光谱，这两个超新星是卡内基超新星计划(CSP)观测到的，与SN1987A有显著的相似性，尽管它们更亮、更蓝、膨胀速度更快。SN2006Au还显示出光曲线的初始倾斜，我们将其解释为冲击爆发的冷却尾巴。通过对每个天体的UVOIR光曲线拟合半解析模型，我们得到了前身的物理性质，我们得出结论：SNE 2006V和2006Au最有可能是蓝色超巨星(BSG)，与SN1987A相比，它们爆炸的能量更大。我们目前正在研究几个BSG SNE的宿主星系，以了解金属丰度在这些罕见的BSG爆炸恒星的产生中所起的作用。
Abstract We studied optical and near-infrared (NIR) light curves, and optical spectra of Supernovae (SNe) 2006V and 2006au, two objects monitored by the Carnegie Supernova Project (CSP) and displaying remarkable similarity to SN 1987A, although they were brighter, bluer and with higher expansion velocities. SN 2006au also shows an initial dip in the light curve, which we have interpreted as the cooling tail of the shock break-out. By fitting semi-analytic models to the UVOIR light curve of each object, we derive the physical properties of the progenitors and we conclude that SNe 2006V and 2006au were most likely Blue Supergiant (BSG) stars that exploded with larger energies as compared to that of SN 1987A. We are currently investigating the host galaxies of a few BSG SNe, in order to understand the role played by the metallicity in the production of these rare exploding BSG stars.