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引用次数: 0
摘要
长期以来,尘埃中的流不稳定性(SI)一直被认为是原行星盘(PPDs)中行星形成的诱发过程。在这项研究中,我们首次对垂直分层盘中的流不稳定性和尘埃凝结过程进行了数值模拟。我们的模拟结果表明,即使最初的尘埃粒径较小,由于尘埃凝结促进了尘埃粒径的增长,SI 最终仍然会被触发。具体来说,尘埃凝结仅受尘埃碎裂的限制,拓宽了以往利用单一尘埃物种进行 SI 研究得出的参数边界。我们描述了尘埃动力学的各个阶段及其大小演变,并探讨了不同尘埃破碎速度的影响。我们还讨论了这些结果对现实 PPD 的影响。
Effects of Dust Coagulation on Streaming Instability
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.