Demographics of Planetesimals Formed by the Streaming Instability
AffiliationUniv Arizona, Steward Observ
Univ Arizona, Dept Astron
methods: data analysis
planets and satellites: formation
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationRixin Li et al 2019 ApJ 885 69
RightsCopyright © 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractThe streaming instability (SI) is a mechanism to aerodynamically concentrate solids in protoplanetary disks and facilitate the formation of planetesimals. Recent numerical modeling efforts have demonstrated the increasing complexity of the initial mass distribution of planetesimals. To better constrain this distribution, we conduct SI simulations including self-gravity with the highest resolution hitherto. To subsequently identify all of the self-bound clumps, we develop a new clump-finding tool, Planetesimal Analyzer. We then apply a maximum likelihood estimator to fit a suite of parameterized models with different levels of complexity to the simulated mass distribution. To determine which models are best-fitting and statistically robust, we apply three model selection criteria with different complexity penalties. We find that the initial mass distribution of clumps is not universal regarding both the functional forms and parameter values. Our model selection criteria prefer models different from those previously considered in the literature. Fits to multi-segment power-law models break to a steeper distribution above masses close to those of 100 km collapsed planetesimals, similar to observed size distributions in the Kuiper Belt. We find evidence for a turnover at the low-mass end of the planetesimal mass distribution in our high-resolution run. Such a turnover is expected for gravitational collapse, but had not previously been reported.
VersionFinal published version
SponsorsNASA headquarters under the NASA Earth and Space Science Fellowship ProgramNational Aeronautics & Space Administration (NASA) [NNX16AP53H]; NASA Astrophysics Theory Grant [NNX17AK59G]; NSFNational Science Foundation (NSF) [AST-1616929]