Formation of planetesimals via the streaming instability - numerical simulations -

流动不稳定性是克服层流中固体颗粒长大为星子障碍的一种机制。因此，这是一个可行的机制，以弥补行星形成理论中的空白。通过流动不稳定性，粒子可以聚集在致密的细丝中，其中引力不稳定的粒子团形成星子。目前，汉堡天文台的博士生UrsSch“afer正在进行数值模拟，以研究流动不稳定性形成各种圆盘性质的星子的效率。这是一个新的数值方法，包括在全球模拟与FLASH代码的中心星星的引力势。

The streaming instability is a mechanism to overcome the barriers impeding the growth of solid particles to planetesimals in laminarflows. It is thus a viable mechanism to close a gap in the theory of planet formation. Via the streaming instability, particles can beconcentrated in dense filaments, in which gravitationally unstable particle clumps form planetesimals. Currently, the PhD student UrsSch\"afer at the Hamburg Observatory is performing numerical simulations to investigate the efficiency of the streaming instability to form planetesimals for various disc properties. This is done with a novel numerical approach including the gravitational potential of thecentral star in global simulations with the FLASH code.