arXiv 2008.131692020-08astro-ph.SRastro-ph.HE

超新星爆炸与非球面拱星物质的相互作用：对光变曲线、谱线轮廓和偏振的影响

Supernova explosions interacting with aspherical circumstellar material: implications for light curves, spectral line profiles, and polarization

P. Kurfürst, O. Pejcha, J. Krtička

发表信息：: A&A 642, A214 (2020)
DOI：: 10.1051/0004-6361/202039073

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摘要：

一些超新星爆发在其光变曲线、谱线轮廓和偏振特征中显示出与预先存在的非球对称星周介质（CSM）相互作用的证据。为了更好地理解与双星的连接，并帮助解释的意见，我们进行二维轴对称流体动力学模拟，其中一个不断扩大的球形SN喷出物初始化与现实的密度和速度分布碰撞各种非球面CSM分布。我们认为CSM的形式是一个拱星盘，碰撞的风壳在双星与不同的方向和距离的SN祖，和双极叶代表缩小版本的侏儒星云的$η$ ~车。我们研究我们的模拟映射到可观的，包括近似的光变曲线，指示性谱线配置文件在晚些时候，和估计的偏振签名。我们发现，SN-CSM碰撞层是由正激波和斜激波，反射波，以及其他流体动力学现象，导致加速和剪切不稳定性。因此，总的冲击加热功率随时间波动，虽然新兴的光变曲线可能是平滑的，如果冲击相互作用区深深地嵌入在SN包络。具有拱星盘或双极瓣的SNe表现出相对于静止速度对称的晚期谱线轮廓和相对高的偏振。相比之下，SNe与碰撞的风壳自然会导致线剖面与不对称和时间演变的蓝色和红色的翅膀和低偏振。由于大质量恒星之间的双星频率很高，SN喷出物与预先存在的碰撞风壳的相互作用必须发生，观测到的签名可以用来描述双星伴星。

英文摘要：

Some supernova (SN) explosions show evidence for interaction with pre-existing non-spherically symmetric circumstellar medium (CSM) in their light curves, spectral line profiles, and polarization signatures. To better understand the connection with binary stars and to aid in the interpretation of observations, we perform two-dimensional axisymmetric hydrodynamic simulations where an expanding spherical SN ejecta initialized with realistic density and velocity profiles collide with various aspherical CSM distributions. We consider CSM in the form of a circumstellar disk, colliding wind shells in binary stars with different orientations and distances from the SN progenitor, and bipolar lobes representing a scaled down version of the Homunculus nebula of $η$~Car. We study how our simulations map onto observables, including approximate light curves, indicative spectral line profiles at late times, and estimates of polarization signature. We find that the SN--CSM collision layer is composed of normal and oblique shocks, reflected waves, and other hydrodynamical phenomena that lead to acceleration and shear instabilities. As a result, the total shock heating power fluctuates in time, although the emerging light curve might be smooth if the shock interaction region is deeply embedded in the SN envelope. SNe with circumstellar disks or bipolar lobes exhibit late-time spectral line profiles symmetric with respect to the rest velocity and relatively high polarization. In contrast, SNe with colliding wind shells naturally lead to line profiles with asymmetric and time-evolving blue and red wings and low polarization. Given the high frequency of binaries among massive stars, interaction of SN ejecta with a pre-existing colliding wind shell must occur and the observed signatures could be used to characterize the binary companion.

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