Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors
Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors
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DOI：
10.3847/2041-8213/acb25e
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发表时间：
2023-01
期刊：
影响因子：
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通讯作者：
K. Maeda;T. Michiyama;P. Chandra;S. Ryder;H. Kuncarayakti;D. Hiramatsu;M. Imanishi
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文献类型：
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作者：
K. Maeda;T. Michiyama;P. Chandra;S. Ryder;H. Kuncarayakti;D. Hiramatsu;M. Imanishi
对超新星（SNe）同步辐射的长期观测，涵盖了爆炸后一年多的时间，提供了一个独特的机会，通过质量损失率的变化来研究大质量恒星在其生命的最后一千年中鲜为人知的演化。在这里，我们提出了我们的长期监测的特殊类型IIL SN 2018 ivc使用阿塔卡马大型毫米/亚毫米阵列的结果。在最初的衰变之后，它在爆炸后2001年开始显示出前所未有的重新明亮。这是在同步辐射中显示这种再增亮的罕见例子之一，也是在毫米波长下的第一个例子。我们发现它是在光学薄制度，不像光学厚厘米发射。这样，我们就可以有力地重建星周物质的分布，从而重建最后1000年的质量损失历史。我们发现SN 2018 ivc的前身在爆炸前约1500年经历了非常高的质量损失率（10−3 M yr−1），随后是中等高的质量损失率（10−4 M yr−1），直到爆炸。根据这种行为，我们认为SN 2018 ivc代表了向SNe IIb演化的极端版本，它将贫氢SNe（向SNe Ib/c，没有氢包层）和富氢SNe（SNe IIP，有大质量包层）连接起来。
Long-term observations of synchrotron emission from supernovae (SNe), covering more than a year after the explosion, provide a unique opportunity to study the poorly understood evolution of massive stars in the final millennium of their lives via changes in the mass-loss rate. Here we present a result of our long-term monitoring of the peculiar Type IIL SN 2018ivc using the Atacama Large Millimeter/submillimeter Array. Following the initial decay, it showed unprecedented rebrightening starting ∼1 yr after the explosion. This is one of the rare examples showing such rebrightening in the synchrotron emission and the first case at millimeter wavelengths. We find it to be in the optically thin regime, unlike the optically thick centimeter emission. As such, we can robustly reconstruct the distribution of the circumstellar matter and thus the mass-loss history in the final ≳1000 yr. We find that the progenitor of SN 2018ivc had experienced a very high mass-loss rate (≳10−3 M ⊙ yr−1) ∼1500 yr before the explosion, which was followed by a moderately high mass-loss rate (≳10−4 M ⊙ yr−1) up until the explosion. From this behavior, we suggest that SN 2018ivc represents an extreme version of a binary evolution toward SNe IIb, which bridges the hydrogen-poor SNe (toward SNe Ib/c, without a hydrogen envelope) and hydrogen-rich SNe (SNe IIP, with a massive envelope).