Early light curves of Type II supernovae interacting with a circumstellar disc
Early light curves of Type II supernovae interacting with a circumstellar disc
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DOI：
10.1093/mnras/staa2360
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发表时间：
2020-08
影响因子：
4.8
通讯作者：
T. Nagao;K. Maeda;R. Ouchi
中科院分区：
文献类型：
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作者：
T. Nagao;K. Maeda;R. Ouchi
II型超新星（SNe）与盘状星周物质（CSM）的相互作用被认为是一些不寻常的II型超新星的解释，例如，所谓的“不可能”SN，iPTF 14 hls。有一些辐射流体动力学模拟这样的SNe与CSM盘相互作用。然而，迄今为止，这种盘相互作用模型还没有包括SN喷出物中的电离和复合过程的影响，即，IIP SNe型的光球层在10 ~ 100天之间受氢复合锋的调节。我们计算了IIP型SNe与CSM盘相互作用的光变曲线，并考察了盘密度和张角对其光变曲线的影响。本文将Moriya等人（2013）的激波相互作用模型嵌入Kasen & Woosley（2009）的IIP型SN模型中，以考虑SN喷出物中电离和复合的影响。我们证明，这种相互作用的SNe显示三个阶段，具有不同的光度和光谱特性，在能源的变化：爆炸后的前几十天（第一阶段），$\sim 10 - \sim 100$天（第二阶段）和天后（第三阶段）。从计算中，我们得出结论，这种隐藏的CSM磁盘不能占过亮型IIP SNe。我们发现，相位1和相位2之间的光度比的信息上的CSM盘的张角。因此，我们鼓励早期的光度和光谱观测相互作用SNe调查其CSM几何。
Type II supernovae (SNe) interacting with disklike circumstellar matter (CSM) have been suggested as an explanation of some unusual Type II SNe, e.g., the so-called "impossible" SN, iPTF14hls. There are some radiation hydrodynamics simulations for such SNe interacting with a CSM disk. However, such disk interaction models so far have not included the effect of the ionization and recombination processes in the SN ejecta, i.e., the fact that the photosphere of Type IIP SNe between $\sim 10$-$\sim 100$ days is regulated by the hydrogen recombination front. We calculate light curves for Type IIP SNe interacting with a CSM disk viewed from the polar direction, and examine the effects of the disk density and opening angle on their bolometric light curves. This work embeds the shock interaction model of Moriya, et al. (2013) within the Type IIP SN model of Kasen & Woosley (2009), for taking into account the effects of the ionization and recombination in the SN ejecta. We demonstrate that such interacting SNe show three phases with different photometric and spectroscopic properties, following the change in the energy source: First few tens days after explosion (Phase 1), $\sim 10 - \sim 100$ days (Phase 2) and days after that (Phase 3). From the calculations, we conclude that such hidden CSM disk cannot account for overluminous Type IIP SNe. We find that the luminosity ratio between Phase 1 and Phase 2 has information on the opening angle of the CSM disk. We thus encourage early photometric and spectroscopic observations of interacting SNe for investigating their CSM geometry.