Dust destruction by supernovae is one of the main processes removing dust from the interstellar medium (ISM). Estimates of the efficiency of this process, both theoretical and observational, typically assume a shock propagating into a homogeneous medium, whereas the ISM possesses significant substructure in reality. We self-consistently model the dust and gas properties of the shocked ISM in three supernova remnants (SNRs), using X-ray and infrared (IR) data combined with corresponding emission models. Collisional heating by gas with properties derived from X-ray observations produces dust temperatures too high to fit the far-IR fluxes from each SNR. An additional colder dust component is required, which has a minimum mass several orders of magnitude larger than that of the warm dust heated by the X-ray emitting gas. Dust-to-gas mass ratios indicate that the majority of the dust in the X-ray emitting material has been destroyed, while the fraction of surviving dust in the cold component is plausibly close to unity. As the cold component makes up virtually all the total dust mass, destruction timescales based on homogeneous models, which cannot account for multiple phases of shocked gas and dust, may be significantly overestimating actual dust destruction efficiencies, and subsequently underestimating grain lifetimes.

中文翻译：

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重新审视超新星的尘埃破坏效率

超新星对尘埃的破坏是从星际介质 (ISM) 中去除尘埃的主要过程之一。对该过程效率的理论和观察估计通常假设冲击传播到均匀介质中，而 ISM 在现实中拥有重要的子结构。我们使用 X 射线和红外 (IR) 数据结合相应的发射模型，自洽地模拟了三个超新星遗迹 (SNR) 中受到冲击的 ISM 的尘埃和气体特性。具有源自 X 射线观测的特性的气体碰撞加热会产生过高的尘埃温度，无法适应每个 SNR 的远红外通量。需要额外的较冷尘埃成分，其最小质量比由 X 射线发射气体加热的温暖尘埃的质量大几个数量级。粉尘与气体的质量比表明 X 射线发射材料中的大部分粉尘已被破坏，而冷成分中幸存的粉尘比例似乎接近于 1。由于冷成分几乎构成了总尘埃质量的全部，基于同质模型的破坏时间尺度无法解释冲击气体和尘埃的多个阶段，可能会大大高估实际的尘埃破坏效率，从而低估颗粒的寿命。