AffiliationUniv Arizona, Steward Observ
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PublisherIOP PUBLISHING LTD
CitationPROMPT PLANETESIMAL FORMATION BEYOND THE SNOW LINE 2016, 828 (1):L2 The Astrophysical Journal Letters
Rights© 2016. The American Astronomical Society. All rights reserved.
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AbstractWe develop a simple model to predict the radial distribution of planetesimal formation. The model is based on the observed growth of dust to millimeter-sized particles, which drift radially, pile-up, and form planetesimals where the stopping time and dust-to-gas ratio intersect the allowed region for streaming instability-induced gravitational collapse. Using an approximate analytic treatment, we first show that drifting particles define a track in metallicity-stopping time space whose only substantial dependence is on the disk's angular momentum transport efficiency. Prompt planetesimal formation is feasible for high particle accretion rates (relative to the gas, (M) over dot(p)/(M) over dot greater than or similar to 3 x 10(-2) for alpha = 10(-2)), which could only be sustained for a limited period of time. If it is possible, it would lead to the deposition of a broad and massive belt of planetesimals with a sharp outer edge. Numerically including turbulent diffusion and vapor condensation processes, we find that a modest enhancement of solids near the snow line occurs for centimeter-sized particles, but that this is largely immaterial for planetesimal formation. We note that radial drift couples planetesimal formation across radii in the disk, and suggest that considerations of planetesimal formation favor a model in which the initial deposition of material for giant planet cores occurs well beyond the snow line.
VersionFinal published version
SponsorsNASA [NNX13AI58G, NNX16AB42G]; NSF AAG grant AST ; NSF AAG grant ; California Institute of Technology (Caltech); Jet Propulsion Laboratory (JPL) - NASA through the Sagan Fellowship Program