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arXiv 2008.11404astro-ph.HE
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快蓝光瞬变AT2018Cow模型：脉动对不稳定性超新星的星周相互作用

A Model for Fast Blue Optical Transient AT2018Cow: Circumstellar Interaction of a Pulsational Pair-instability Supernova

Shing-Chi Leung, Sergei Blinnikov, Ken'ichi Nomoto, Petr Baklanov, Elena Sorokina, Alexey Tolstov

备注：
17 pages, 31 figures, published in Astrophysical Journal, submitted at 7 February 2020, accepted at 18 September 2020, published at 3 November 2020
发表信息：
Astrophysical Journal 903, 66 (2020)
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摘要：

ATLAS 18qqn（AT2018cow）的光变曲线与超亮超新星一样明亮，但上升和下降速度要快得多。我们在前人研究的PPISN模型的基础上，通过脉动对不稳定性（PPI）超新星（SN）模型的星周相互作用来模拟这种光变曲线。我们专注于42 $M_\odot$ He星（80 $M_{\odot}$星的核心），它有质量为0.50 $M_\odot$的拱星物质。利用参数化的质量截断和爆炸动能$E$，我们对PPISN模型的核合成和光学光变曲线进行了流体力学计算。用$E = 5 \times 10^{51}$ erg对$42 ~M_{\odot}$ He星的星周物质进行激波加热，很好地再现了AT2018 cow的第一个$\sim$ 20天的光学光变曲线.在第20天之后，通过0.6 $M_\odot$ $^{56}$ Co的放射性衰变再现光变曲线，该放射性衰变是$^{56}$ Ni在爆炸中的衰变产物。我们还研究了光变曲线形状如何取决于各种模型参数，如CSM结构和组成。我们还讨论了（1）其他可能的能源及其限制，（2）所观察到的高能辐射的起源，以及（3）我们的结果如何依赖于辐射传递代码。基于我们成功的AT 2018奶牛模型和CSM质量与$20 ~M_\odot)$一样大的SLSN模型，我们提出了工作假设，即如果CSM质量足够大，PPISN会产生SLSNe，如果CSM小于$\sim 1 ~M_\odot$，则会产生FBOTs。

英文摘要：

The Fast Blue Optical Transient (FBOT) ATLAS18qqn (AT2018cow) has a light curve as bright as superluminous supernovae but rises and falls much faster. We model this light curve by circumstellar interaction of a pulsational pair-instability (PPI) supernova (SN) model based on our PPISN models studied in previous work. We focus on the 42 $M_\odot$ He star (core of a 80 $M_{\odot}$ star) which has circumstellar matter of mass 0.50 $M_\odot$. With the parameterized mass cut and the kinetic energy of explosion $E$, we perform hydrodynamical calculations of nucleosynthesis and optical light curves of PPISN models. The optical light curve of the first $\sim$ 20 days of AT2018cow is well-reproduced by the shock heating of circumstellar matter for the $42 ~M_{\odot}$ He star with $E = 5 \times 10^{51}$ erg. After day 20, the light curve is reproduced by the radioactive decay of 0.6 $M_\odot$ $^{56}$Co, which is a decay product of $^{56}$Ni in the explosion. We also examine how the light curve shape depends on the various model parameters, such as CSM structure and composition. We also discuss (1) other possible energy sources and their constraints, (2) origin of observed high-energy radiation, and (3) how our result depends on the radiative transfer codes. Based on our successful model for AT2018cow and the model for SLSN with the CSM mass as large as $20 ~M_\odot)$, we propose the working hypothesis that PPISN produces SLSNe if CSM is massive enough and FBOTs if CSM is less than $\sim 1 ~M_\odot$.

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