Computer Science – Sound
Scientific paper
Oct 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.0406w&link_type=abstract
American Astronomical Society, DPS meeting #42, #4.06; Bulletin of the American Astronomical Society, Vol. 42, p.948
Computer Science
Sound
Scientific paper
In the giant impact model of lunar formation (Cameron & Ward 1976), the Earth is surrounded by a debris disk composed primarily of silicate material immediately following the impact event (e.g., Canup 2004). The dynamical evolution of the disk is driven by gravitational instabilities that generate an effective viscosity, causing the disk to spread (Ward & Cameron 1978; Takeda & Ida 2001). A portion of the material expands across the Roche boundary where it can eventually accrete into the Moon, while the remaining material is re-accreted by the Earth. The spreading rate is regulated by the disk's radiation budget through a complex two-phase gas/magna equilibrium state that maintains the radiation temperature near 2000 K (Thompson & Stevenson 1988). The vertical structure of the disk must satisfy the Clausius-Clapeyron phase equilibrium equation as well as equations of hydrostatic and convective equilibrium. The two phase disk has a modified sound speed that depends on the mass fractions of gas versus liquid, and consequently, there is a range of possible structures that depend on these fractions. We will examine under what conditions different disk structures are likely to have prevailed during the early history of the system. The resulting consequences of various disk histories on the dynamics and timing of the Moon's accretion will also be considered.
This research is supported by funds from the NASA Lunar Science Institute (NLSI) and from NASA's LASER program.
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