A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction
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DOI：
10.3847/1538-4357/aca1b7
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发表时间：
2022-11
期刊：
影响因子：
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通讯作者：
K. Maeda;P. Chandra;T. Moriya;A. Reguitti;S. Ryder;T. Matsuoka;T. Michiyama;G. Pignata;
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文献类型：
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作者：
K. Maeda;P. Chandra;T. Moriya;A. Reguitti;S. Ryder;T. Matsuoka;T. Michiyama;G. Pignata;
SN 2018 ivc是一颗不寻常的II型超新星（SN II）。它是SNe IIL的一个变体，可能代表了SNe IIP和SNe IIb之间的过渡情况，前者有大量的富氢包层，后者只有少量的富氢包层。然而，SN 2018 ivc的光学光变曲线演化比典型的SNe IIL更复杂。在本文中，我们提出了及时的后续观测SN 2018 ivc与阿塔卡马大型毫米/亚毫米阵列的结果。它的同步辐射类似于SN IIb 1993 J，这表明它本质上是一颗氦星星的类似SN IIb的爆炸，具有适度（10.5 - 1 M）的富氢扩展包层。它的无线电，光学和X射线光变曲线主要是由SN喷出物和拱星物质（CSM）之间的相互作用来解释的;因此，我们认为这是一个罕见的例子（第一个涉及“规范”SN IIb喷出物），其中多波长发射主要由SN-CSM相互作用提供动力。内部CSM的密度，反映了最后十年的祖先活动，与SN IIb 2013 cu的密度相当，显示出闪光光谱特征。外层CSM的密度，以及在最后200年的质量损失率，比SN 1993 J高出10.5倍。我们认为，SN 2018 ivc代表了SNe IIP和SNe IIb/Ib/Ic在二进制演化情景中缺失的链接。
SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb–like explosion of an He star with a modest (∼0.5–1M ⊙) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN–CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.