SN 1987 A光回波$-$ AT2019xis的辐射转移模拟
Radiative Transfer Modeling of An SN 1987A Light Echo$-$AT2019xis
摘要：
本文利用蒙特卡罗辐射转移模型（MCRTM）模拟了大麦云云（LMC）中超新星SN $~$ 1987 A的UBVRI光变曲线、图像和光回波的线偏振。我们比较的理论模拟的AT 2019轴，光回波检测到一个大的角距离（4.05 $^{'}$）从SN $~$ 1987 A的观测。利用光学引力透镜实验（OGLE-IV）瞬态探测系统（OTDS）的I波段光变曲线，结合数值模拟结果，估算了沙尘云的大小和光学厚度。尘埃云的质量是使用估计的大小，光学厚度和消光系数计算的。如果假设尘埃云对应的气尘比为300，则尘埃云的总质量约为7.8-9.3 $M_{\odot}$。基于这些理论模型，我们表明，在波长范围内或短于U波段的光回波的形态形状是非常不同的那些在较长的波长波段，和差异进行的SN $~$ 1987 A的早期紫外辐射的重要信息。
英文摘要：
We use a Monte Carlo radiative transfer model (MCRTM) to simulate the UBVRI light curves, images and linear polarization of a light echo from supernova SN$~$1987A in the Large Magellanic Cloud (LMC) using various dust cloud shapes, sizes, and optical properties. We compare the theoretical simulations to the observations of AT2019xis, a light echo detected at a large angular distance (4.05$^{'}$) from SN$~$1987A. We estimate the size and optical thickness of the dust cloud based on the simulation results and the observations of Optical Gravitational Lensing Experiment (OGLE-IV) Transient Detection System (OTDS) I-band light curve. The mass of the dust cloud is calculated using the estimated size, optical thickness and extinction coefficient. If the dust cloud is assumed to correspond to a gas-to-dust ratio of 300, the total mass of the dust cloud is approximately 7.8-9.3 $M_{\odot}$. Based on these theoretical models, we show that the morphological shapes of the light echoes in the wavelength range in or shorter than the U-band to be very different from those in the longer wavelength bands, and the difference carries important information on the early UV radiation of SN$~$1987A.
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