Abstract
We review the dynamical processes in accretion of the Moon from an impact-generated disk, based on the results of direct N-body simulations. The important processes are tidal inhibition of accretion within the Roche limit, development of density spiral arms, radial migration of disk mass associated with angular momentum transfer by the spiral arms, formation of particle aggregates by self-gravity, and interaction of formed moonlets with the disk. As a result of the disk evolution, a single large moon is formed at about 3–4R⊕ on a time scale of a month to a year, in most cases. The mass of the formed moon is regulated by the total mass and angular momentum of the initial disk.
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Ida, S., Kokubo, E., Takeda, T. (2001). N-Body Simulations of Moon Accretion. In: Marov, M.Y., Rickman, H. (eds) Collisional Processes in the Solar System. Astrophysics and Space Science Library, vol 261. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0712-2_13
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DOI: https://doi.org/10.1007/978-94-010-0712-2_13
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