标题： 利用超新星1992A的晚期光曲线检验前体模型 显示英文标题

标题： Testing Progenitor Models Using the Late-Time Light Curve of Supernova 1992A

摘要： 驱动Ia型超新星光变曲线的主要放射性能量来源预计将在非常晚的阶段从 $^{56}$Co 衰变切换到 $^{57}$Co 衰变。 我们使用在爆炸后超过900天获得的SN1992A的存档HST图像来限制其钴同位素丰度比，并将其与研究得很好的事件SN2011fe进行比较。 我们确认了SN2011fe的 $^{57}$Co / $^{56}$Co 比值为 $0.026\pm 0.004$，这与“双致密星”前身星模型一致，该结果来自arXiv:1608.01155。 对于SN1992A，我们发现比值为 $0.034\pm 0.010$，但较大的不确定性不允许我们区分前身星模型。 显示英文摘要

摘要： The dominant radioactive energy source powering Type Ia supernova light curves is expected to switch from the decay of $^{56}$Co to $^{57}$Co at very late epochs. We use archival HST images of SN1992A obtained more than 900 days after explosion to constrain its cobalt isotopic abundance ratio and compare it to the well-studied event SN2011fe. We confirm the $^{57}$Co / $^{56}$Co ratio for SN2011fe of $0.026\pm 0.004$ found by arXiv:1608.01155, consistent with a "double degenerate" progenitor scenario. For SN1992A, we find a ratio of $0.034\pm 0.010$, but the large uncertainty does not allow us to differentiate between progenitor models