The Peculiar Type Ib Supernova 2006jc: A WCO Wolf-Rayet Star Explosion
The Peculiar Type Ib Supernova 2006jc: A WCO Wolf-Rayet Star Explosion
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DOI：
10.1086/591782
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发表时间：
2007-11
期刊：
影响因子：
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通讯作者：
N. Tominaga;M. Limongi;M. Limongi;Tomoharu Suzuki;Masaomi Tanaka;K. Nomoto;K. Nomoto;K. Maeda-K.-Maed
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文献类型：
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作者：
N. Tominaga;M. Limongi;M. Limongi;Tomoharu Suzuki;Masaomi Tanaka;K. Nomoto;K. Nomoto;K. Maeda-K.-Maed
我们提出了Ib型超新星（SN） 2006jc的理论模型。我们计算了原恒星的演化，SN爆炸的流体力学和核合成，以及SN的热光度曲线（LC）。将合成的热通量液相色谱与紫外、光学、近红外和中红外光谱相结合构建的热通量液相色谱进行了比较。它的前身被假定质量为40 M☉，位于零年龄主序上。这颗恒星经历了大量的质量损失，使其质量降至6.9 M☉，从而成为WCO沃尔夫-拉叶星。WCO星模型具有较厚的富碳层，其中可以形成无定形碳颗粒。这可以解释近红外光谱中的增亮和MIR光谱中的尘埃特征。我们认为SN 2006jc的祖先是一颗WCO Wolf-Rayet恒星，经历了强烈的质量损失，这种大质量恒星是尘埃形成的重要场所。我们推导了爆炸模型的参数，以便通过放射性衰变重现SN 2006jc的热量LC：喷出物质量4.9 M☉，超超新星样爆炸能量1052 ergs，喷出物56Ni质量0.22 M☉。我们还计算了星周相互作用，发现要重现SN 2006jc的x射线LC，需要具有平坦密度结构的CSM。这表明质量损失率和/或风速的剧烈变化与过去的发光蓝变量（LBV）事件一致。
We present a theoretical model for Type Ib supernova (SN) 2006jc. We calculate the evolution of the progenitor star, hydrodynamics and nucleosynthesis of the SN explosion, and the SN bolometric light curve (LC). The synthetic bolometric LC is compared with the observed bolometric LC constructed by integrating the UV, optical, near-infrared (NIR), and mid-infrared (MIR) fluxes. The progenitor is assumed to be as massive as 40 M☉ on the zero-age main sequence. The star undergoes extensive mass loss to reduce its mass down to as small as 6.9 M☉, thus becoming a WCO Wolf-Rayet star. The WCO star model has a thick carbon-rich layer, in which amorphous carbon grains can be formed. This could explain the NIR brightening and the dust feature seen in the MIR spectrum. We suggest that the progenitor of SN 2006jc is a WCO Wolf-Rayet star having undergone strong mass loss, and such massive stars are important sites of dust formation. We derive the parameters of the explosion model in order to reproduce the bolometric LC of SN 2006jc by the radioactive decays: the ejecta mass 4.9 M☉, hypernova-like explosion energy 1052 ergs, and ejected 56Ni mass 0.22 M☉. We also calculate the circumstellar interaction and find that a CSM with a flat density structure is required to reproduce the X-ray LC of SN 2006jc. This suggests a drastic change of the mass-loss rate and/or the wind velocity that is consistent with the past luminous blue variable (LBV)-like event.