重新审视0/I类原恒星盘中的尘埃碰撞增长：在0.1 Myr内扫掠式增长可将数十个地球质量的尘埃转化为千克级卵石
Revisiting collisional dust growth in Class 0/I protostellar disks: Sweep-up can convert a few $10 M_\oplus$ of dust into kg pebbles in 0.1 Myr
AI总结：
本文通过颗粒凝聚计算研究0/I类原恒星盘中的尘埃碰撞增长，发现扫掠式增长机制可在0.1 Myr内将约50个地球质量的尘埃转化为千克级卵石，远超碎裂势垒，且该卵石群体对星子形成和行星核心质量预算具有重要意义。
摘要：
近期观测表明，行星形成的最初阶段可能发生在年轻恒星天体演化的0/I类阶段，此时恒星和盘仍嵌入在坍缩包层中。在本研究中，我们进行颗粒凝聚计算，以研究0/I类盘中行星形成的最初阶段，即尘埃颗粒的碰撞增长。我们发现，通过与远小于自身的颗粒发生高速碰撞而实现的颗粒质量缓慢增长（“扫掠式增长”）使得约50个地球质量的颗粒在0/I类阶段结束时（0.1 Myr）能够远超碎裂势垒，增长为约千克级的卵石。我们分析了扫掠式增长的线性增长和饱和过程，以定量理解我们的结果，并检验扫掠式增长的结果是否对盘参数和颗粒凝聚模型的细节敏感。扫掠式增长的卵石群体可能对行星形成很重要，因为它们与气体的耦合较弱（相比于碎裂势垒以下的主要群体），因此更有利于已知的尘埃团块形成机制（这些机制启动星子形成）。根据对行星质量预算的观测估计，该群体还包含足以形成所有行星核心的质量。我们的发现为未来研究0/I类盘中的颗粒增长和星子形成提供了动力，包括这一扫掠式增长群体的后续演化。
英文摘要：
Recent observations suggest that the first stages of planet formation likely take place in the Class 0/I phase of Young Stellar Object evolution, when the star and the disk are still embedded in an infalling envelope. In this study we perform grain coagulation calculations to investigate the very first stage of planet formation, the collisional growth of dust grains, in Class 0/I disks. We find that the slow increase in grain mass by high-velocity collision with much smaller grains ("sweep-up") allows $\sim 50 M_\oplus$ of grains to grow well beyond the fragmentation barrier into $\sim$kg pebbles by the end of Class 0/I (0.1 Myr). We analyze the linear growth and saturation of sweep-up to understand our results quantitatively, and test whether the sweep-up outcome is sensitive to disk parameters and details of the grain coagulation model. The sweep-up pebble population could be important for planet formation, because they are less well-coupled to the gas (compared to the main population below the fragmentation barrier) and therefore more favorable to known mechanisms of dust clump formation (which initiate planetesimal formation). It also contains enough mass to form all planet cores, based on observational estimates of the planet mass budget. Our findings motivate future studies of grain growth and planetesimal formation in Class 0/I disks, including the subsequent evolution of this sweep-up population.
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