Streaming instability (SI) in dust has long been thought to be a promising process in triggering planetesimal formation in the protoplanetary disks (PPDs). In this study, we present the first numerical investigation that models the SI in the vertically stratified disk together with the dust coagulation process. Our simulations reveal that, even with the initially small dust sizes, because dust coagulation promotes dust size growth, SI can eventually still be triggered. Specifically, dust coagulation, limited only by dust fragmentation, broadens the parameter boundaries obtained from previous SI studies using single dust species. We describe the various stages of dust dynamics along with their size evolution and explore the impact of different dust fragmentation velocities. Implications of these results for realistic PPDs are also discussed.

中文翻译：

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尘埃凝结对流不稳定性的影响


长期以来，尘埃中的流不稳定性 （SI） 一直被认为是触发原行星盘 （PPD） 中行星体形成的一个有前途的过程。在这项研究中，我们提出了第一个数值研究，该研究模拟了垂直分层盘中的 SI 以及灰尘凝结过程。我们的模拟表明，即使最初尘埃量很小，由于尘埃凝结会促进尘量的增长，最终仍然可以触发 SI。具体来说，仅受粉尘碎裂限制的粉尘凝结拓宽了从先前使用单一粉尘种类的 SI 研究中获得的参数边界。我们描述了尘埃动力学的各个阶段及其大小演变，并探讨了不同尘埃碎裂速度的影响。还讨论了这些结果对现实 PPD 的影响。