论文标题
使用1+1d近似值在原星盘中热表面波的模拟
Simulations of thermal surface waves in a protoplanetary disk using 1+1D approximation
论文作者
论文摘要
中央恒星的加热是决定原月球磁盘物理结构的关键因素之一。由于径向方向上的光学厚度较大，因此磁盘中平面区域通过磁盘表面的红外辐射（大气）加热，而红外辐射又是由恒星直接加热的。以前证明，磁盘表面上不均匀性对恒星辐射的拦截会引起扰动，从而向恒星传播。在这项工作中，我们调查了原动性磁盘详细的1D数值模型中此类波的发生。我们证实了先前的发现，在磁盘中，光学厚到其自身的辐射，表面扰动确实发生并传播到恒星。但是，与某些分析预测相反，足够大的磁盘中的热波仅影响上层，而中平面中温度的显着波动。我们的结果表明，有必要在更一致的流体动力模型中研究这种不稳定。
Heating by the central star is one of the key factors determining the physical structure of protoplanetary disks. Due to the large optical thickness in the radial direction, disk midplane regions are heated by the infrared radiation from the disk surface (atmosphere), which in turn is directly heated by the star. It was previously shown that interception of the stellar radiation by inhomogeneities on the disk surface can cause perturbations that propagate towards the star. In this work, we investigate the occurrence of such waves within a detailed 1+1D numerical model of the protoplanetary disk. We confirm the previous findings that in the disk, that is optically thick to its own radiation, the surface perturbations indeed occur and propagate towards the star. However, contrary to some analytical predictions, the thermal waves in sufficiently massive disks affect only the upper layers without significant fluctuations of temperature in the midplane. Our results indicate the need to study this instability within more consistent hydrodynamic models.
