Radio Observations of Six Young Type Ia Supernovae
Radio Observations of Six Young Type Ia Supernovae
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DOI：
10.3847/1538-4357/acd84f
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发表时间：
2023-05
期刊：
影响因子：
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通讯作者：
C. Harris;S. Sarbadhicary;L. Chomiuk;A. Piro;D. Sand;S. Valenti
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文献类型：
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作者：
C. Harris;S. Sarbadhicary;L. Chomiuk;A. Piro;D. Sand;S. Valenti
Ia型超新星(SNE Ia)是重要的宇宙学工具，是双星演化的探测器，也是宇宙金属丰度的贡献者；然而，对产生它们的双星系统的确切理解仍然是难以捉摸的。特别令人感兴趣的是，质量供体伴星与正在爆炸的碳氧白矮星(COWD)的身份。在这项工作中，我们介绍了由Jansky甚大天线阵拍摄的六个附近(40Mpc内)SNE Ia的早期(爆炸后10天内的第一次观测)射电观测，这些观测被用来限制来自抛射物和星周物质(CSM)相互作用的同步辐射的存在。这些早期观测的两个动机是：(1)限制低密度风的存在和(2)为那些观测到可能由CSM相互作用引起的SNE Ia早期光学/UV过剩提供另一种研究途径。我们没有探测到任何目标的无线电发射。对于我们的第一个目标，这些未探测到的天体进一步增加了SNE Ia的样本，排除了来自共生双星和强烈吸积的白矮星的风。并讨论了对基本模式假设的依赖，以及我们的观测如何表示具有低密度风约束的SNE Ia样本的大幅增加。对于第二个目标，我们提供了一个辐射流体动力学模拟来研究SN Ia与CSM致密壳层相互作用的射电发射，发现尽管激波爆发后激波壳层迅速膨胀，相对论电子却不能存活下来产生射电发射。讨论了模型假设对风和紧凑型壳体结论的影响。
Type Ia supernovae (SNe Ia) are important cosmological tools, probes of binary star evolution, and contributors to cosmic metal enrichment; yet, a definitive understanding of the binary star systems that produce them remains elusive. Of particular interest is the identity of the mass-donor companion to the exploding carbon–oxygen white dwarf (CO WD). In this work, we present early-time (first observation within 10 days post-explosion) radio observations of six nearby (within 40 Mpc) SNe Ia taken by the Jansky Very Large Array, which are used to constrain the presence of synchrotron emission from the interaction between ejecta and circumstellar material (CSM). The two motivations for these early-time observations are: (1) to constrain the presence of low-density winds and (2) to provide an additional avenue of investigation for those SNe Ia observed to have early-time optical/UV excesses that may be due to CSM interaction. We detect no radio emission from any of our targets. Toward our first aim, these non-detections further increase the sample of SNe Ia that rule out winds from symbiotic binaries and strongly accreting white dwarfs. and discuss the dependence on underlying model assumptions and how our observations represent a large increase in the sample of SNe Ia with low-density wind constraints. For the second aim, we present a radiation hydrodynamics simulation to explore radio emission from an SN Ia interacting with a compact shell of CSM, and find that relativistic electrons cannot survive to produce radio emission despite the rapid expansion of the shocked shell after shock breakout. The effects of model assumptions are discussed for both the wind and compact shell conclusions.