解开超新星尘埃的起源和加热机制：I型超新星的晚期Spitzer光谱学In SN 2005 ip
Disentangling the Origin and Heating Mechanism of Supernova Dust: Late-Time Spitzer Spectroscopy of the Type IIn SN 2005ip
摘要：
本文介绍了NGC 2906中SN 2005 ip中I型暖尘埃的晚期近红外和{ \it Spitzer}中红外光度和光谱观测。光谱显示了两种不同温度的尘埃成分的证据。这些观测跨越热发射的峰值，对尘埃质量、温度和亮度提供了强有力的约束，这些约束可以作为解开每个成分的起源和加热机制的关键诊断。结果表明，较温暖的尘埃质量为$\sim 5 \times 10^{-4}~$ \msolar，起源于喷出物中新形成的尘埃，或可能是冷的致密壳层，并通过星周相互作用持续加热。相比之下，较冷的成分可能来自于一个星周激波回波，它是由一个大的、预先存在的尘埃壳层$\sim 0.01 - 0.05$ ~ \msolar ~被后期的星周相互作用加热而形成的。从He 1 1.083 \micron ~P天鹅座轮廓的蓝色边缘获得的祖先风速表明，在超新星爆炸前100年，祖先喷发可能形成了这个尘埃壳层$\sim$，这与亮蓝变星（LBV）的祖先星一致。
英文摘要：
This paper presents late-time near-infrared and {\it Spitzer} mid-infrared photometric and spectroscopic observations of warm dust in the Type IIn SN 2005ip in NGC 2906. The spectra show evidence for two dust components with different temperatures. Spanning the peak of the thermal emission, these observations provide strong constraints on the dust mass, temperature, and luminosity, which serve as critical diagnostics for disentangling the origin and heating mechanism of each component. The results suggest the warmer dust has a mass of $\sim 5 \times 10^{-4}~$\msolar, originates from newly formed dust in the ejecta, or possibly the cool, dense shell, and is continuously heated by the circumstellar interaction. By contrast, the cooler component likely originates from a circumstellar shock echo that forms from the heating of a large, pre-existing dust shell $\sim 0.01 - 0.05$~\msolar~by the late-time circumstellar interaction. The progenitor wind velocity derived from the blue edge of the He 1 1.083 \micron~P Cygni profile indicates a progenitor eruption likely formed this dust shell $\sim$100 years prior to the supernova explosion, which is consistent with a Luminous Blue Variable (LBV) progenitor star.
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