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N-Body Dynamics as a Mechanism for Mean Motion Resonance Formation in the Post-Gas Era — arXiv:2609.31244

Source: arXiv (en)
Original: https://arxiv.org/abs/2609.31244
License (as archived): CC0-1.0
Archived: 2026-10-08T04:12:08.252Z
SHA-256 of the archived text: ad24d796bea96df93c50cc1f4f33ec2b8993914ec1d6a71c0564a9e2650ad037
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How to cite

N-Body Dynamics as a Mechanism for Mean Motion Resonance Formation in the Post-Gas Era — arXiv:2609.31244 — arXiv (en), https://arxiv.org/abs/2609.31244 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_ab80dffcaa44 (Metraipolis archive dc_ab80dffcaa44, sha256 ad24d796bea96df93c50cc1f4f33ec2b8993914ec1d6a71c0564a9e2650ad037)

BibTeX

@misc{dcab80dffcaa44,
  title = {N-Body Dynamics as a Mechanism for Mean Motion Resonance Formation in the Post-Gas Era — arXiv:2609.31244},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2609.31244},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_ab80dffcaa44; sha256 ad24d796bea96df93c50cc1f4f33ec2b8993914ec1d6a71c0564a9e2650ad037},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2609.31244. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Mean motion resonances (MMRs) are traditionally thought to form during the gas-rich phase of protoplanetary disks via disk-driven migration. Whether MMRs can form solely through collisional damping after disk dispersal has not been systematically investigated. To study MMR formation in the post-gas-disk era, we perform a large suite of N-body simulations, each containing 10,000 planetesimals around an M-dwarf star and evolving over 10 Myr. We compare two groups of simulations that differ only in their initial mass distributions. Each group consists of 10 runs with statistically identical initial planetesimal orbital distributions, generated using different random seeds. One group adopts a uniform planetesimal mass distribution, whereas the other features a bimodal distribution with massive embryos embedded in a swarm of smaller planetesimals. At 1 Myr, 40% of systems (8/20) exhibit near-resonant period ratios, but this fraction drops to 25% (5/20) by 10 Myr as higher-order commensurabilities dissolve. Resonant-angle tracking shows that all persistent systems have circulating resonant angles at 10 Myr, although one system undergoes a transient libration phase between about 2 and 7 Myr before returning to circulation. These results demonstrate that collisional merging can drive MMR formation even without a gas disk, although in this scenario near-resonant configurations are strongly favored over true resonances. Furthermore, this mechanism produces similar MMR fractions in both groups, suggesting that MMR formation is insensitive to the initial mass distribution, although the latter may modulate the formation pathway to a limited extent.

Tema degli esploratori: fisica e astronomia (retro-catalogo arXiv: annunci del 2026-09-28 in astro-ph.EP).
Categorie arXiv: Earth and Planetary Astrophysics (astro-ph.EP).
Pagina del lavoro: https://arxiv.org/abs/2609.31244 — autori e testo completo sono lì (qui omessi i nomi: nessun dato personale nel deposito).
Licenza: titolo e abstract sono metadati arXiv distribuiti in CC0 1.0; il testo completo ha la licenza scelta dagli autori, indicata sulla pagina.
Letto il 2026-10-08T03:37:40.653Z dalla pagina https://arxiv.org/catchup/astro-ph.EP/2026-09-28?abs=True (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).