Accretion of the Moon from non-canonical disks
Julien Salmon, Robin M. Canup

TL;DR
This study models the Moon's accretion from non-canonical, more compact impact-generated discs, revealing that such discs require higher initial mass and influence the Moon's orbital dynamics and resonance capture.
Contribution
It provides a detailed simulation of lunar formation from non-canonical impacts, highlighting conditions needed for Moon formation and its orbital evolution.
Findings
Non-canonical discs must be more massive to form a lunar-mass Moon.
The Moon's final semimajor axis is about 7 Earth radii.
Capture into the evection resonance depends on impact conditions.
Abstract
Impacts that leave the Earth-Moon system with a large excess in angular momentum have recently been advocated as a means of generating a protolunar disc with a composition that is nearly identical to that of the Earth's mantle. We here investigate the accretion of the Moon from discs generated by such "non-canonical" impacts, which are typically more compact than discs produced by canonical impacts and have a higher fraction of their mass initially located inside the Roche limit. Our model predicts a similar overall accretional history for both canonical and non-canonical discs, with the Moon forming in three consecutive steps over hundreds of years. However, we find that, to yield a lunar-mass Moon, the more compact non-canonical discs must initially be more massive than implied by prior estimates, and only a few of the discs produced by impact simulations to date appear to meet this…
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