基于AKARI近中红外观测的SN2006jc新形成尘埃的性质
Properties of newly formed dust by SN2006jc based on near-to-mid infrared observation with AKARI
摘要：
本文介绍了我们利用$AKARI$上的红外照相机（IRC）在发现SN 2006 jc后200天对它进行近中红外观测的最新结果。首次获得了SN 2006 jc的近红外（2- 5 $μ$ m）光谱，并发现该光谱与超新星喷出物中形成的质量为$6.9\pm 0.5 \times 10^{-5}M_{\odot}$、温度为800 $\pm 10$ K的无定形碳的热辐射很好地解释。在SN 2006 jc的喷出物中新形成的尘埃团与根据最近的观测获得的其他几个尘埃形成核心塌陷超新星的范围相似（即，$10^{-3}$ -- $10^{-5}$ $M_{\odot}$）。使用{ \it{AKARI} }/IRC MIR-S/S7、S9 W和S11波段的中红外测光数据表明，在800 K的热无定形碳的热发射上有过量的发射。这种中红外过量发射可能是由质量为2.7 $^{+0.7}_{-0.5} \times 10^{-3}M_{\odot}$的320 $\pm 10$ K的温暖无定形碳尘埃的发射造成的，而不是天文硅酸盐和/或二氧化硅颗粒的带发射。这种温暖的无定形碳尘埃预计是在SN爆炸前与沃尔夫-拉叶恒星活动相关的质量损失风中形成的。我们的研究结果表明，大量的尘埃是在SN爆炸前的质量损失风凝聚。本文还提出了在7.5- 9.5PDMATHABMN m范围内，晶体SiO分子对发射带的贡献。
英文摘要：
We present our latest results on near- to mid- infrared observation of SN2006jc at 200 days after the discovery using the Infrared Camera (IRC) on board $AKARI$. The near-infrared (2--5$μ$m) spectrum of SN2006jc is obtained for the first time and is found to be well interpreted in terms of the thermal emission from amorphous carbon of 800$\pm 10$K with the mass of $6.9\pm 0.5 \times 10^{-5}M_{\odot}$ that was formed in the supernova ejecta. This dust mass newly formed in the ejecta of SN 2006jc is in a range similar to those obtained for other several dust forming core collapse supernovae based on recent observations (i.e., $10^{-3}$--$10^{-5}$$M_{\odot}$). Mid-infrared photometric data with {\it{AKARI}}/IRC MIR-S/S7, S9W, and S11 bands have shown excess emission over the thermal emission by hot amorphous carbon of 800K. This mid-infrared excess emission is likely to be accounted for by the emission from warm amorphous carbon dust of 320$\pm 10$K with the mass of 2.7$^{+0.7}_{-0.5} \times 10^{-3}M_{\odot}$ rather than by the band emission of astronomical silicate and/or silica grains. This warm amorphous carbon dust is expected to have been formed in the mass loss wind associated with the Wolf-Rayet stellar activity before the SN explosion. Our result suggests that a significant amount of dust is condensed in the mass loss wind prior to the SN explosion. A possible contribution of emission bands by precursory SiO molecules in 7.5--9.5$μ$m is also suggested.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
