原行星盘中的风蚀：它对尘埃演化的影响有多大？
Aeolian erosion in protoplanetary discs: How impactful it is on dust evolution?
AI总结：
本文通过一维和三维模型模拟，发现风蚀在考虑径向漂移、碎裂和尘埃陷阱时对原行星盘尘埃演化影响可忽略，但可能影响后期阶段。
摘要：
背景：许多障碍阻碍了尘埃通过原行星盘中的凝聚形成星子，例如弹跳、碰撞碎裂或风蚀。因此，需要对尘埃以及可能改变其演化的各种现象进行建模。目前已提出了多种解决方案，但仍需确认。目的：在本文中，我们探讨风蚀在尘埃演化中所起的作用。方法：我们使用单分散模型来考虑尘埃的生长和碎裂，该模型被实现在一维模型中用以计算单个颗粒的演化，并使用三维SPH代码来计算尘埃和气体的全局演化。我们在代码中测试了侵蚀模型，并确保其与先前的结果一致。结果：使用一个再现观测的盘模型，我们通过一维和三维研究均表明，在考虑碎裂的情况下，侵蚀在尘埃演化过程中并不显著。在低黏度盘中，碎裂问题较小，但颗粒生长也较不重要，这无论如何都阻止了大天体的形成。在靠近恒星的尘埃陷阱中，即使关闭碎裂，侵蚀也影响不大。结论：我们在本文中表明，当考虑径向漂移、碎裂和尘埃陷阱时，风蚀是可忽略的，并且不会改变盘中的尘埃演化。然而，它可能对后期阶段产生影响，即当流不稳定性在恒星附近形成大团块时，或当星子被捕获时。
英文摘要：
Context: Many barriers prevent dust to form planetesimals via coagulation in protoplanetary discs, such as bouncing, collisional fragmentation or aeolian erosion. Modelling dust and the different phenomena that can alter its evolution is therefore needed. Multiple solutions have been proposed, but still need to be confirmed. Aims: In this paper, we explore the role aeolian erosion plays in the evolution of dust. Methods: We use a monodisperse model to account for dust growth and fragmentation, implemented in a 1D model to compute the evolution of single grains and a 3D SPH code to compute the global evolution of dust and gas. We test the erosion model in our code and ensured it matches previous results. Results: With a model of disc reproducing observations, we show with both 1D and 3D studies that erosion is not significant during the evolution of dust when we take fragmentation into consideration. With a low-viscosity disc, fragmentation is less of a problem, but grain growth is also less important, preventing the formation of large objects anyway. In dust traps, close to the star, erosion is also not impactful, even when fragmentation is turned off. Conclusions: We show in this paper that aeolian erosion is negligible when radial drift, fragmentation and dust traps are taken into account and does not alter the dust evolution in the disc. However, it can have an impact on later stages, i.e. when the streaming instability forms large clumps close to the star, or when planetesimals are captured.
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