Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...617..633m&link_type=abstract
The Astrophysical Journal, Volume 617, Issue 1, pp. 633-644.
Astronomy and Astrophysics
Astronomy
5
Hydrodynamics, Instabilities, Moon, Planets And Satellites: Formation
Scientific paper
We have performed a two-phase fluid numerical simulation of the evolution of a partially vaporized circumplanetary disk. In the giant-impact hypothesis, gravitational instability is crucial for the moon-forming process. It causes outward transportation of disk material beyond the Roche radius, where the disk material can accrete into a moon. There are two possible modes of gravitational instability: one is the instability of the melt-vapor mixture following disk cooling, and the other is the instability of the equatorial melt layer formed by sedimentation in the disk. In this paper, we examine the latter possibility, which has been poorly understood. The major results obtained are as follows: (1) The sedimentation of melt droplets occurs in about 10-2 yr, which is much faster than the disk cooling (~100 yr). (2) The gravitational instability of the melt layer occurs when the gas fraction is below the critical value (~0.7). When the gas fraction exceeds the critical value, neither type of gravitational instability occurs. These results suggest that the constituent of the melt layer is transported beyond the Roche radius much faster than the disk cooling unless the gas fraction is extremely high. As a consequence, a volatile-poor moon is expected to be formed while the disk still remains hot.
Abe Yutaka
Machida Ryosuke
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