论文标题
与早期互动的超新星中的薄薄外壳中的灰尘产生
Dust Production in a Thin Dense Shell in Supernovae with Early Circumstellar Interactions
论文作者
论文摘要
在Supernovae（SNE）中，光曲线显示出射出和偶然物质（CSM）之间强烈和早期相互作用的证据，据估计，新粉尘的形成是在正向（FS）和反向冲击（RS）之间的密集的气体外壳中发生的。在这项研究中，首次对这种致密壳中的灰尘形成机理进行了建模。考虑了弹出质量的变化和前探索质量损失率的一组9例，这是考虑到该SNE中报道的相互作用的多样性的。对于单个主序列质量，射流质量的变化表现为恒星H壳质量的变化，由于前探索质量损失而丢失。我们发现，密集外壳中的尘埃质量范围在10 $^{ - 3} $ m $ _ {\ odot} $和0.8 m $ _ {\ odot} $的0.8 m $ _ {\ odot} $中，由O富含O富含O和C的晶粒组成，其相对比例取决于交互的性质。震后气体中的灰尘形成的特征是逐渐生产速率，从10 $^{ - 6} $到10 $^{ - 3} $ M $ _ {\ odot} $ DAY $^{ - 1} $，可能会持续十年，十年后进行证明。较高的质量降低速率会导致较大的灰尘，而较小的喷射质量（较小的左H-壳）会提高这种SNE的粉尘产生效率。如我们的计算中，在RS后面形成的灰尘不会受到FS或RS的破坏，因此可能比在喷射中形成的灰尘更大的比例生存。
In supernovae (SNe), where the light curves show evidence of strong and early interaction between the ejecta and the circumstellar matter (CSM), the formation of new dust is estimated to take place in a dense shell of gas between the forward (FS) and the reverse shock (RS). For the first time, in this study, the mechanism of dust formation in this dense shell is modeled. A set of 9 cases, considering variations of the ejecta mass, and the pre-explosion mass-loss rates is considered, accounting for the diverse nature of interactions reported in such SNe. For a single main sequence mass, the variation of ejecta mass was manifested as a variation of the H-shell mass of the star, lost due to pre-explosion mass-loss. We find that the dust masses in the dense shell range between 10$^{-3}$ M$_{\odot}$ and 0.8 M$_{\odot}$, composed of O-rich and C-rich grains, whose relative proportions are determined by the nature of interaction. Dust formation in the post-shock gas is characterized by a gradual production rate, mostly ranging from 10$^{-6}$ to 10$^{-3}$ M$_{\odot}$ day$^{-1}$, which may continue for a decade, post-explosion. A higher mass-loss rate leads to a larger mass of dust, while a smaller ejecta mass (smaller left-over H-shell) increases the efficiency of dust production in such SNe. Dust formed behind the RS, as in our calculations, is not subject to destruction by either the FS or RS and is thus likely to survive in larger proportion than dust formed in the ejecta.
