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首页> 外文期刊>The Astrophysical journal >DUST FORMATION AND He II λ4686 EMISSION IN THE DENSE SHELL OF THE PECULIAR TYPE Ib SUPERNOVA 2006jc
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DUST FORMATION AND He II λ4686 EMISSION IN THE DENSE SHELL OF THE PECULIAR TYPE Ib SUPERNOVA 2006jc

机译：特异型Ib超新星2006jc的致密壳中的尘埃形成和He IIλ4686排放

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摘要

We present evidence for the formation of dust grains in an unusual Type 1b supernova (SN) based on late-time spectra of SN 2006jc. The progenitor suffered an outburst qualitatively similar to those of luminous blue variables (LBVs) just 2 yr prior to the SN, and we propose that the dust formation is a consequence of the SN blast wave overtaking that LBV-like shell. The key evidence for dust formation is (1) the appearance of a red ear-infrared continuum emission source that can be fit by T ≈ 1600 K graphite grains, and (2) fading of the redshifted sides of intermediate-width He I emission lines, yielding progressively more asymmetric blueshifted lines as dust obscures receding material. This provides the strongest case yet for dust formation in any SN Ib/c. Both developments occurred between 51 and 75 days after peak brightness, while the few other SNe observed to form dust did so after a few hundred days. Geometric considerations indicate that dust formed in the dense swept-up shell between the forward and reverse shocks, and not in the freely expanding SN ejecta. The rapid cooling leading to dust formation may have been aided by extremely high shell densities of 10~(10) cm~(-3), indicated by He i line ratios. The brief epoch of dust formation is accompanied by He n λ4686 emission and enhanced X-ray emission, suggesting a common link. These clues imply that the unusual dust formation in this object was not attributable to properties of the SN itself, but instead-like most peculiarities of SN 2006jc-was a consequence of interaction with the dense environment created by an LBV-like eruption 2 yr before the SN.
机译：我们根据SN 2006jc的后期光谱，为不寻常的1b型超新星（SN）中的尘埃颗粒形成提供了证据。祖细胞的爆发在质量上与SN前2年的发光蓝色变量（LBV）相似，我们认为尘埃形成是SN爆炸波超过LBV样壳的结果。形成尘埃的关键证据是：（1）出现了一个红色/近红外连续发射源，可以适合T≈1600 K石墨晶粒;（2）中等宽度He I发射的红移边逐渐褪色。线，随着灰尘遮盖后退材料，逐渐产生更多不对称的蓝移线。这为任何SN Ib / c中的粉尘形成提供了最有力的理由。两种发展都发生在峰值亮度之后的51到75天之间，而观察到的形成尘埃的其他少数SNe则在几百天后发生了。几何上的考虑表明，在向前和向后的冲击之间，在密集的扫掠壳中形成了粉尘，而在自由扩展的SN射流中则没有形成粉尘。快速冷却导致形成粉尘可能是由He i线比表示的极高的10〜（10）cm〜（-3）的壳密度所辅助的。尘埃形成的短暂时期伴随着He nλ4686发射和增强的X射线发射，暗示了一个共同的联系。这些线索表明，该物体中异常粉尘的形成并非归因于SN本身的特性，而是像SN 2006jc的大多数特殊特征一样，是与2年前LBV样喷发所形成的稠密环境相互作用的结果。 SN。

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