论文标题
核心偏曲超新星和富含CA的瞬变中的氧和钙nebular发射线关系
Oxygen and calcium nebular emission line relationships in core-collapse supernovae and Ca-rich transients
论文作者
论文摘要
这项工作检查了[O I] $λλ$ 6300，6364，[Ca II] $λλ$ 7291，7323和Ca II近帧近汇的三胞胎，核心核心超级群体的发射行，以及86（s s s s s s s semplase offermant offrared supplet）（s s s s s s semplase offrared triplet）（s s s s s sements cromptions offrared sumplet''的属性（通量比，全宽度为一半速度）之间的关系之间的关系。 10个瞬态是富含CA的事件）。研究了线条频率比作为时间的函数，与瞬态类别之间的差异进行了差异，特别是发现II型SNE具有与剥离的Envelope（SE）SNE相比具有不同的线条频率比。在Se-Sne的[Ca II]/[O I]通量比之间未发现相关性，它们的弹出质量和动能（如光曲线建模所测量），这表明在更发光的Se-Sne中可能会产生附加电源的贡献。我们发现，[Ca II]发射线的平均特征宽度小于所有SN类型的[O I]发射线，表明[Ca II]发射通常源自[O IXPTA中的更深层，而不是[O I]。这与II型SNE排放的标准模型有些紧张。还将II型SNE的发射线属性与理论模型进行了比较，并发现有利于较低的质量轨道（$ M_ \ Mathrm {Zams} $ $ <$ <$ 15 m $ _ $ _ {\ odot} $），没有证据表明$^{56} $ ni将其混合到H eNvelope中，也没有大量混合到O壳中。发现某些级级别SNE的通量比与Se-Sne相似，而Se-Sne的缩放比例可以考虑到其更长的上升时间（尽管我们警告样本量很小）。
This work examines the relationships between the properties (flux ratios, full width at half-maximum velocities) of the [O I] $λλ$6300, 6364, [Ca II] $λλ$7291, 7323, and the Ca II near-infrared triplet, emission lines of a large sample of core-collapse supernovae (SNe) and Ca-rich transients (509 spectra of 86 transients, of which 10 transients are Ca-rich events). Line-flux ratios as a function of time were investigated with differences identified between the transient classes, in particular the Type II SNe were found to have distinct line-flux ratios compared to stripped-envelope (SE) SNe. No correlation was found between the [Ca II]/[O I] flux ratios of SE-SNe and their ejecta masses and kinetic energies (as measured from light curve modelling), suggesting that there may be a contribution from an additional power source in more luminous SE-SNe. We found that the mean characteristic width of the [Ca II] emission line is less than the [O I] emission line for all SN types, indicating that the [Ca II] emission typically originates from deeper in the ejecta than [O I]. This is in some tension with standard models for emission in Type II SNe. The emission line properties of Type II SNe were also compared to theoretical models and found to favour lower mass tracks ($M_\mathrm{ZAMS}$ $<$ 15 M$_{\odot}$), with no evidence found for significant mixing of $^{56}$Ni into the H envelope nor Ca mixed into the O shell. The flux ratios of some superluminous SNe were found to be similar to those of SE-SNe when scaling to account for their longer rise times was applied (although we caution the sample size is small).
