Rapid Dust Growth During Hydrodynamic Clumping Due to Streaming Instability
Ryosuke T. Tominaga, Hidekazu Tanaka

TL;DR
This paper investigates how dust grains grow rapidly during the early stages of streaming instability-induced clumping, highlighting the significance of local coagulation before strong dust clumping occurs in planetesimal formation.
Contribution
It provides the first estimate of dust growth timescales during the pre-clumping phase of streaming instability, emphasizing the role of coagulation in planetesimal formation.
Findings
Dust growth occurs significantly before strong clumping begins.
Moderate clumping raises local dust-to-gas ratio above 10.
Dust collision velocities can be maintained below 1 m/s, facilitating safe growth.
Abstract
Streaming instability is considered to be one of the dominant processes to promote planetesimal formation by gravitational collapse of dust clumps. The development of streaming instability is expected to form dust clumps in which the local dust density is strongly enhanced and even greater than the Roche density. The resulting clumps can collapse to form planetesimals. Recent simulations conducted long-term simulations and showed that such strong clumping occurs in a wider parameter space than previously expected. However, the indicated timescale for strong clumping can be on the order of tens to hundreds Keplerian periods. In this paper, we estimate the growth time of dust grains during the pre-clumping phase. We find that the dust growth considerably proceeds before the strong clumping because even the moderate clumping due to streaming instability increases the local dust-to-gas…
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Taxonomy
TopicsAstrophysics and Star Formation Studies · Astro and Planetary Science · Spacecraft and Cryogenic Technologies
