In the standard model of terrestrial planet formation, planets are formed through giant impacts of planetary embryos after the dispersal of the protoplanetary gas disc.
Traditionally, N-body simulations have been used to investigate this process. However, they are computationally too expensive to generate sufficient planetary populations for statistical comparisons with observational data. A previous study introduced a semi-analytical model that incorporates the orbital and accretionary evolution of planets due to giant impacts and gravitational scattering.
This model succeeded in reproducing the statistical features of planets in N-body simulations near 1 au around solar-mass stars. However, this model is not applicable to close-in regions (around 0.1 au) or low-mass stars because the dynamical evolution of planetary systems depends on the orbital radius and stellar mass. This study presents a new semi-analytical model applicable to close-in orbits around stars of various masses, validated through comparison with N-body simulations.
The model accurately predicts the final distributions of planetary mass, semi-major axis, and eccentricity for the wide ranges of orbital radius, initial planetary mass, and stellar mass, with significantly reduced computation time compared to N-body simulations. By integrating this model with other planet-forming processes, a computationally low-cost planetary population synthesis model can be developed.
Tadahiro Kimura, Haruka Hoshino, Eiichiro Kokubo, Yuji Matsumoto, Masahiro Ikoma
Comments: 16 pages, 9 figures, 1 table, accepted for publication in ApJ
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2505.20548 [astro-ph.EP](or arXiv:2505.20548v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2505.20548
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Submission history
From: Tadahiro Kimura
[v1] Mon, 26 May 2025 22:22:55 UTC (341 KB)
https://arxiv.org/abs/2505.20548
Astrobiology,
