论文标题
原行星磁盘中流型不稳定性的物理模型
Physical models of streaming instabilities in protoplanetary disks
论文作者
论文摘要
我们为阻力引起的尘埃流流不稳定性开发了简单的，有动机的模型，这对于将晶粒块形成恒星磁盘中的行星很重要。这些模型基于气态环球运动和尘埃拖曳力的物理学，这是流媒体不稳定性的最重要特征及其简单的概括，即磁盘沉降不稳定性。我们模型解释的一些关键特性包括当尘埃气质量比超过1时，流质不稳定性的生长速率突然变化，与较小的谷物的沉降不稳定性相比，流媒体不稳定的缓慢增长速度以及在不同机制中最不稳定模式的生长的主要物理过程。除了提供有用的简化图片，以了解有趣且基本的天体物理流体不稳定性的运行外，我们的模型还可能被证明可用于分析模拟和开发磁盘中行星生长的非线性理论。
We develop simple, physically motivated models for drag-induced dust-gas streaming instabilities, which are thought to be crucial for clumping grains to form planetesimals in protoplanetary disks. The models explain, based on the physics of gaseous epicyclic motion and dust-gas drag forces, the most important features of the streaming instability and its simple generalisation, the disk settling instability. Some of the key properties explained by our models include the sudden change in the growth rate of the streaming instability when the dust-to-gas-mass ratio surpasses one, the slow growth rate of the streaming instability compared to the settling instability for smaller grains, and the main physical processes underlying the growth of the most unstable modes in different regimes. As well as providing helpful simplified pictures for understanding the operation of an interesting and fundamental astrophysical fluid instability, our models may prove useful for analysing simulations and developing nonlinear theories of planetesimal growth in disks.
