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arXiv 1809.09055astro-ph.SRastro-ph.GA
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在SN 2005年IP中I型喷出物尘埃形成的十年

A decade of ejecta dust formation in the Type IIn SN 2005ip

A. Bevan, R. Wesson, M. J. Barlow, I. De Looze, J. E. Andrews, G. C. Clayton, K. Krafton, M. Matsuura, D. Milisavljevic

备注：
Accepted by MNRAS, 17 pages, 11 figures. Author accepted manuscript. Accepted on 04/03/19. Deposited on 07/03/19
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摘要：

为了了解核心坍缩超新星对早期宇宙尘埃收支的贡献，重要的是不仅要了解核心坍缩超新星中可能形成的尘埃质量，还要了解尘埃形成的位置和速度。SN 2005 ip特别令人感兴趣，因为尘埃被推断为在辐射反向激波后面的喷出物和激波后区域形成。我们整理了八个跨越SN 2005 ip寿命的光学档案光谱，并在发现后4075天提出了SN 2005 ip的新X-射手光学近红外光谱。使用Monte Carlo线传输代码DAMOCLES，我们已经模拟了蓝移宽和中间宽度H $α$，H $β$和He I线从48天到4075天后发现使用喷出物尘埃模型。我们发现，喷出物中的灰尘可以解释在宽和中间宽度H $α$，H $β$和He I线配置文件中观察到的不对称性在所有的时代，它是没有必要调用后冲击尘埃形成来解释在中间宽度后冲击线观察到的蓝移。使用贝叶斯方法，我们已经确定了在SN 2005 IP的喷出物尘埃质量的演变超过10年假设喷出物尘埃模型，增加的尘埃质量从~10 $^{-8}$ M $_{\odot}$在48天到目前的尘埃质量的$\sim$ 0.1 M $_{\odot}$。

英文摘要：

In order to understand the contribution of core-collapse supernovae to the dust budget of the early universe, it is important to understand not only the mass of dust that can form in core-collapse supernovae but also the location and rate of dust formation. SN 2005ip is of particular interest since dust has been inferred to have formed in both the ejecta and the post-shock region behind the radiative reverse shock. We have collated eight optical archival spectra that span the lifetime of SN 2005ip and we additionally present a new X-shooter optical-near-IR spectrum of SN 2005ip at 4075d post-discovery. Using the Monte Carlo line transfer code DAMOCLES, we have modelled the blueshifted broad and intermediate width H$α$, H$β$ and He I lines from 48d to 4075d post-discovery using an ejecta dust model. We find that dust in the ejecta can account for the asymmetries observed in the broad and intermediate width H$α$, H$β$ and He I line profiles at all epochs and that it is not necessary to invoke post-shock dust formation to explain the blueshifting observed in the intermediate width post-shock lines. Using a Bayesian approach, we have determined the evolution of the ejecta dust mass in SN 2005ip over 10 years presuming an ejecta dust model, with an increasing dust mass from ~10$^{-8}$ M$_{\odot}$ at 48d to a current dust mass of $\sim$0.1 M$_{\odot}$.

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