论文标题
在中子星合并的光球处的爆炸浪潮出现的第一原则模拟
A first-principle simulation of blast wave emergence at the photosphere of a neutron star merger
论文作者
论文摘要
我们介绍了在相对论流出的光球处出现的辐射介导的冲击的第一个从头算模拟。使用我们的代码辐射进行仿真，该代码radshock遵循使用蒙特卡洛方法计算的时间依赖性辐射转移的流体动力学。我们使用代码检查中子星合并GW〜170817的辐射爆炸波。以前有人提出合并弹出了一个黑暗的，相对扩展的，同源的包膜，然后在包膜内爆炸产生了观察到的伽马射线爆发GRB 〜170817a。我们的模拟说明了冲击波通过包膜传播，接近光球，释放辐射并崩溃时，如何产生辐射，并分成两个微观厚度的无碰撞冲击。我们发现光曲线和产生的伽马射线爆发的光谱演变；两者都类似于观察到的grb〜170817a。
We present the first ab initio simulation of a radiation-mediated shock emerging at the photosphere of a relativistic outflow. The simulation is performed using our code radshock that follows fluid dynamics coupled to time-dependent radiative transfer, calculated with the Monte-Carlo method. We use the code to examine the radiative blast wave emerging from neutron star merger GW~170817. It was previously proposed that the merger ejected a dark, relativistically expanding, homologous envelope, and then an explosion inside the envelope produced the observed gamma-ray burst GRB~170817A. Our simulation demonstrates how the shock wave generates radiation as it propagates through the envelope, approaches its photosphere, releases the radiation, and collapses, splitting into two collisionless shocks of a microscopic thickness. We find the light curve and the spectral evolution of the produced gamma-ray burst; both are similar to the observed GRB~170817A.
