论文标题
最大最大的光谱良好的贫于氢的超浮肿超新星多样性
Pre-maximum spectroscopic diversity of hydrogen-poor superluminous supernovae
论文作者
论文摘要
我们搜索在最大最大相位的氢贫血超级新星（SLSNE-I）的光谱多样性背后的原因。我们的分析是\ citet {ktr21}论文的延续，他披露了两个新的Slsne-I亚型，其特征是在其4000至5000Å之间的最大最大光谱中存在W形吸收特征（分别称为〜W和类型〜150亿）。但是，这种双峰性的物理原因仍然不确定。在这里，我们提出27 slsne-i的最大最大光谱合成，并特别注意光谱温度（$ t_ {\ rm phot} $）和速度（$ v_ {\ rm phot} $）。我们发现，$ t _ {\ rm phot} $限制为12000〜K可以分开〜w和type〜15bn slsne-i：type〜w对象倾向于显示$ t _ {\ rm phot} \ geq $ 12000〜K，而类型〜150亿只有$ t _ t _ t _ {\ rm Phot} \ rm Phot} \ 12000;这与所研究物体的化学组成一致。这些组之间的另一个区别可以在其射出几何形状中找到：w slsne-i类型可能显示出无效的偏振，这意味着球形对称性，而150亿对象的极化可能会在时间上增加。这表明了一个具有球形外碳氧层和一个不对称的内层具有重离子的两组分模型。 这两个亚组也可能具有不同的光曲线演变，因为6型〜W对象显示早期凸起，这与150亿SLSNE-I类型不同。 但是，此功能需要进一步的研究，因为它仅基于目前的几个对象。
We search for the reasons behind the spectroscopic diversity of hydrogen-poor superluminous supernovae (SLSNe-I) in the pre-maximum phase. Our analysis is a continuation of the paper of \citet{ktr21}, who disclosed two new subtypes of SLSNe-I characterized by the presence/absence of a W-shaped absorption feature in their pre-maximum spectra between 4000 and 5000 Å(called Type~W and Type~15bn, respectively). However, the physical cause of this bimodality is still uncertain. Here we present pre-maximum spectral synthesis of 27 SLSNe-I with special attention to the photospheric temperature ($T_{ \rm phot}$) and velocity ($v_{ \rm phot}$) evolution. We find that a $T_{\rm phot}$ limit of 12000~K separates the Type~W and Type~15bn SLSNe-I: Type~W objects tend to show $T_{\rm phot}\geq$12000~K, while Type~15bn ones have $T_{\rm phot} \leq$12000~K. This is consistent with the chemical composition of the studied objects. Another difference between these groups may be found in their ejecta geometry: Type W SLSNe-I may show null-polarization, implying spherical symmetry, while the polarization of Type 15bn objects may increase in time. This suggests a two-component model with a spherical outer carbon-oxygen layer and an asymmetric inner layer containing heavier ions. The two subgroups may have different light curve evolution as well, since 6 Type~W objects show early bumps, unlike Type 15bn SLSNe-I. This feature, however, needs further study, as it is based on only a few objects at present.
