Tumbling Dice: Radio Constraints on the Presence of Circumstellar Shells around Type Ia Supernovae with Impact Near Maximum Light
Tumbling Dice: Radio Constraints on the Presence of Circumstellar Shells around Type Ia Supernovae with Impact Near Maximum Light
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DOI：
10.3847/1538-4357/abe940
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发表时间：
2021-02
期刊：
影响因子：
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通讯作者：
C. Harris;L. Chomiuk;P. Nugent
中科院分区：
文献类型：
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作者：
C. Harris;L. Chomiuk;P. Nugent
Ia型超新星(SNE Ia)的祖先们一直在争论，尤其是为正在爆炸的碳氧白矮星提供质量的双星伴星的演化状态。在我们以前的工作中，我们给出了SNE Ia与CSM分离的受限壳层相互作用的流体力学模型和光学薄的射电同步光曲线，代表了由新星形成的CSM。在这项工作中，我们将这些光曲线扩展到光学厚区，同时考虑了同步加速器自吸收和自由吸收。我们得到了简单的公式来描述在模拟中看到的光学厚度的演变，允许对任意壳层性质的光学厚光曲线进行近似。然后，我们通过解释已发布的无线电数据来演示此工具的使用。首先，我们考虑了PTF11kx--一种已知具有分离的受限壳层的SN Ia--的未被探测到的情况，我们发现这种未被探测到的情况与其CSM的现有模型是一致的，而且以后的观测对这次事件将是有用的。其次，我们统计分析了没有相互作用特征的SneIa的射电未探测集合。我们发现，质量为(10−4-0.3)M⊙的壳体位于距离前身(1015-1016)cm的位置，由于其昏暗、快速演化的光曲线，目前不能很好地受到射电数据的约束。
The progenitors of Type Ia supernovae (SNe Ia) are debated, particularly the evolutionary state of the binary companion that donates mass to the exploding carbon–oxygen white dwarf. In our previous work, we presented hydrodynamic models and optically thin radio synchrotron light curves of SNe Ia interacting with detached, confined shells of CSM, representing CSM shaped by novae. In this work, we extend these light curves to the optically thick regime, considering both synchrotron self-absorption and free–free absorption. We obtain simple formulae to describe the evolution of optical depth seen in the simulations, allowing optically thick light curves to be approximated for arbitrary shell properties. We then demonstrate the use of this tool by interpreting published radio data. First, we consider the nondetection of PTF11kx—an SN Ia known to have a detached, confined shell—and we find that the nondetection is consistent with current models for its CSM, and that observations at a later time would have been useful for this event. Second, we statistically analyze an ensemble of radio nondetections for SNe Ia with no signatures of interaction. We find that shells with masses (10−4–0.3) M ⊙ located (1015–1016) cm from the progenitor are currently not well constrained by radio datasets, due to their dim, rapidly evolving light curves.