Positive Feedback: How a Synergy Between the Streaming Instability and Dust Coagulation Forms Planetesimals

Abstract

One of the most important open questions in planet formation is how dust grains in a protoplanetary disk manage to overcome growth barriers and form the $\sim$100km planet building blocks that we call planetesimals. There appears to be a gap between the largest grains that can be produce by coagulation, and the smallest grains that are needed for the streaming instability (SI) to form planetesimals. Here we explore a novel hypothesis: That dust coagulation and the SI work in tandem. That they form a feedback loop where each one boosts the action of the other to bridge the gap between dust grains and planetesimals. We develop a semi-analytical model of dust concentration due to the SI, and an analytic model of how the SI affects the fragmentation and radial drift barriers. We then combine those to model our proposed feedback loop. In the fragmentation-limited regime, we find a powerful synergy between the SI and dust growth that drastically increases both grain sizes and densities. We find that a midplane dust-to-gas ratio of $\epsilon \ge 0.3$ is a sufficient condition for the feedback loop to reach the planetesimal-forming region for turbulence values $10^{-4}\le \alpha \le 10^{-3}$ and grain sizes $0.01\le \mathrm{St}\le 0.1$. In contrast, the drift-limited regime only shows grain growth, without significant dust accumulation. Planet formation in the drift-limited portion of the disk may require other processes (particle traps) to halt radial drift.

5 pages, 4 figures, submitted to A&A Letters

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Cited by in corpus (4)

• Effects of Stellar X-ray Photoevaporation on Planetesimal Formation via the Streaming Instability
• Positive Feedback II: How Dust Coagulation inside Vortices Can Form Planetesimals at Low Metallicity
• Evading the dust fragmentation barrier with the streaming instability in protoplanetary disks
• Magnetic clumping of charged dust in the dense interstellar medium