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Peer-reviewedCC BY 4.0The Astrophysical Journal

A Semianalytic Model of the Bouncing Barrier for Protoplanetary Dust Aggregates

  • Sota Arakawa1
  • Haruto Oshiro2
  • Yuki Yoshida3
  • Kiwamu Yoshii4
4 affiliations
  1. 1Japan Agency for Marine-Earth Science and Technology
  2. 2Institute of Science Tokyo
  3. 3Tohoku University
  4. 4Tokyo University of Science
Open at sourcePDFDOICite

Abstract

Collisional bouncing limits the growth of dust aggregates in protoplanetary disks, but its dependence on aggregate size, collision velocity, and filling factor remains poorly understood. Here we develop a semianalytic model for the sticking probability of colliding dust aggregates. We divide each aggregate collision into two phases: a compression phase and a separation phase. The compression phase is described with an elastoplastic contact model, which determines the maximum contact radius and repulsive energy after compression. The separation phase is treated as fracture of a stochastic network of interparticle bonds, whose fracture energy is evaluated using weakest-link statistics. The model naturally predicts that larger aggregates bounce more readily because larger contact regions are more likely to contain weak bonds. Comparison with distinct element method simulations shows that the model reproduces the simulated sticking–bouncing boundary. Furthermore, applying the calibrated model to moderately porous aggregates inferred from Atacama Large Millimeter/submillimeter Array observations of protoplanetary disks, we find that the predicted bouncing barrier passes through the observationally inferred size–velocity range. Thus, our semianalytic model provides a useful framework for predicting the collisional evolution of protoplanetary dust aggregates.

Versions

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Cite

BibTeXRIS
BibTeX
@article{arakawa2026semianalytic,
  title = {{A Semianalytic Model of the Bouncing Barrier for Protoplanetary Dust Aggregates}},
  author = {Sota Arakawa and Haruto Oshiro and Yuki Yoshida and Kiwamu Yoshii},
  journal = {The Astrophysical Journal},
  year = {2026},
  month = oct,
  doi = {10.3847/1538-4357/aea78b},
  url = {https://iopscience.iop.org/article/10.3847/1538-4357/aea78b},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - A Semianalytic Model of the Bouncing Barrier for Protoplanetary Dust Aggregates
AU  - Sota Arakawa
AU  - Haruto Oshiro
AU  - Yuki Yoshida
AU  - Kiwamu Yoshii
PY  - 2026
DA  - 2026/10/12
JO  - The Astrophysical Journal
DO  - 10.3847/1538-4357/aea78b
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/aea78b
AB  - Collisional bouncing limits the growth of dust aggregates in protoplanetary disks, but its dependence on aggregate size, collision velocity, and filling factor remains poorly understood. Here we develop a semianalytic model for the sticking probability of colliding dust aggregates. We divide each aggregate collision into two phases: a compression phase and a separation phase. The compression phase is described with an elastoplastic contact model, which determines the maximum contact radius and repulsive energy after compression. The separation phase is treated as fracture of a stochastic network of interparticle bonds, whose fracture energy is evaluated using weakest-link statistics. The model naturally predicts that larger aggregates bounce more readily because larger contact regions are more likely to contain weak bonds. Comparison with distinct element method simulations shows that the model reproduces the simulated sticking–bouncing boundary. Furthermore, applying the calibrated model to moderately porous aggregates inferred from Atacama Large Millimeter/submillimeter Array observations of protoplanetary disks, we find that the predicted bouncing barrier passes through the observationally inferred size–velocity range. Thus, our semianalytic model provides a useful framework for predicting the collisional evolution of protoplanetary dust aggregates.
SN  - 0004-637X
SN  - 1538-4357
ER  -