论文标题
$γ$ - 富含钙的超新星的沉积历史
The $γ$-ray deposition histories of Calcium-rich supernovae
论文作者
论文摘要
富含钙的超新星（富含CAICH的SNE）是微弱的，快速发展的瞬态，其祖细胞系统尚未确定。我们从文献中得出了五个富含CA的SNE的$γ$ -Ray沉积历史，以便在可能的祖细胞系统上放置约束。我们发现，在IA SNE类型和剥离的信封Supernovae（Sesne）之间的未占用区域内，CA-RICH SNE样本中的$γ$ - Rease Escape Time，$ T_0 $，$ \ t_0 $。 $ t_0 $ - $ m_ \ mathrm {ni56} $分布这些sne，其中$ m_ \ mathrm {ni56} $是爆炸中的合成$^{56} $ ni质量所有事件之间的连接。通过将我们的结果与文献中的模型进行比较，我们能够确定氦壳爆炸模型和超脱落恒星的核心折叠模型不太可能解释Ca-Ca-Ca-Ca-Ca-rich SNE，因为这些模型中的伽马射线逃逸时间小于观察到的值。 Models that agree with the observed $ t_0$-$M_\mathrm{Ni56} $ distribution are explosions of low mass, $M\approx0.75$-$0.8\,M_\odot $, white dwarfs and core-collapse models of stripped stars with an ejecta mass of $M\approx1$-$3\,M_{\odot}$.
Calcium-rich supernovae (Ca-rich SNe) are faint, rapidly evolving transients whose progenitor system is yet to be determined. We derive the $γ$-ray deposition histories of five Ca-rich SNe from the literature in order to place constraints on possible progenitor systems. We find that the $ γ$-ray escape time, $ t_0 $, of the Ca-rich SNe sample is $\approx35$-$65 \,\rm{d}$, within the unoccupied region between Type Ia SNe and stripped envelope supernovae (SESNe). The $ t_0$-$M_\mathrm{Ni56} $ distribution of these SNe, where $M_\mathrm{Ni56}$ is the synthesised $^{56}$Ni mass in the explosion, creates a continuum between the Type Ia and SESNe $ t_0$-$M_\mathrm{Ni56} $ distribution, hinting at a possible connection between all the events. By comparing our results to models from the literature, we were able to determine that helium shell detonation models and core-collapse models of ultra-stripped stars are unlikely to explain Ca-rich SNe, since the gamma-ray escape time in these models is smaller than the observed values. Models that agree with the observed $ t_0$-$M_\mathrm{Ni56} $ distribution are explosions of low mass, $M\approx0.75$-$0.8\,M_\odot $, white dwarfs and core-collapse models of stripped stars with an ejecta mass of $M\approx1$-$3\,M_{\odot}$.
