论文标题
限制核心爆发超新星的早期灰尘形成
Constraining early-time dust formation in core-collapse supernovae
论文作者
论文摘要
目前，核心崩溃超新星（CCSNE）中尘埃形成的理论模型之间存在严重的差异，该模型预测$ \ gtrsim 0.01 $ m $ _ \ odot $ _ \ odot $ odot $ odot $ odot $ odot $ \ sim \ sim 1000 $ 1000 $ $ $ $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ odot。我们证明，在光学薄的情况下，尽管观察到明显的观察和模型不确定性，但这些低尘埃质量仍然健壮。对于11个观察良好的CCSNE的样本，没有合理的模型到达碳灰尘块以上$ 10^{ - 4} $ M $ _ \ odot $，或$ \ sim 10^{ - 3} $ M $ _ $ _ $ _ \ odot $。光学厚的型号可以容纳更大的灰尘块，但是灰尘必须结块，并且覆盖分数的低（$ <0.1 $），以避免与光波长处的数据冲突。这些值不足以再现观察到的红外通量，所需的覆盖分数不仅在同一对象的时期之间，而且在时期之间有所不同。将大型尘埃质量与CCSNE的早期观察结合在一起，再加上超级新星残留物中较大的尘埃质量的探测，这表明有必要形成延迟时间灰尘的机制。
There is currently a severe discrepancy between theoretical models of dust formation in core-collapse supernovae (CCSNe), which predict $\gtrsim 0.01$ M$_\odot$ of ejecta dust forming within $\sim 1000$ days, and observations at these epochs, which infer much lower masses. We demonstrate that, in the optically thin case, these low dust masses are robust despite significant observational and model uncertainties. For a sample of 11 well-observed CCSNe, no plausible model reaches carbon dust masses above $10^{-4}$ M$_\odot$, or silicate masses above $\sim 10^{-3}$ M$_\odot$. Optically thick models can accommodate larger dust masses, but the dust must be clumped and have a low ($<0.1$) covering fraction to avoid conflict with data at optical wavelengths. These values are insufficient to reproduce the observed infrared fluxes, and the required covering fraction varies not only between SNe but between epochs for the same object. The difficulty in reconciling large dust masses with early-time observations of CCSNe, combined with well-established detections of comparably large dust masses in supernova remnants, suggests that a mechanism for late-time dust formation is necessary.
