Direct Numerical Simulation of Comet Impacts and Low-Density Atmospheric Flow on the Moon

Details Direct Numerical Simulation of Comet Impacts and Low-Density Atmospheric Flow on the Moon Direct Numerical Simulation of Comet Impacts and Low-Density Atmospheric Flow on the Moon

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5710l&link_type=abstract

American Astronomical Society, DPS meeting #38, #57.10; Bulletin of the American Astronomical Society, Vol. 38, p.589

Astronomy and Astrophysics

Astronomy

Scientific paper

The present work uses a hybrid numerical method to simulate a comet impact on the Moon and the ensuing rarefied atmosphere. The impact event is simulated using the SOVA hydrocode (Shuvalov 1999) while the expansion atmosphere is simulated using the Direct Simulation Monte Carlo (DSMC) method. The macroscopic data provided by the hydrocode simulation are used as input in the DSMC code to create simulated water molecules. The molecules that are not destroyed due to loss processes such as escape, ionization or dissociation will be followed as they hop around the Moon until they reach a cold trap. After the initial impact event, it is expected that a certain fraction of molecules will be lost to space as their velocity will be larger than the escape velocity. The remaining molecules will fall to the surface and equilibrate to the local surface temperature. The molecules that hit the surface of the Moon on the sunlit side will be released nearly instantaneously while molecules on the dark side will stay on the surface until the dawn terminator reaches their location. Then molecules will continue to bounce until they are destroyed or captured in a cold trap. The present DSMC code has been modified from its previous version in order to run 3D parallel simulations on scalable supercomputers. Hybrid SOVA-DSMC results at the early stages of the impact will be presented for a vertical impact as well as later time DSMC results showing the evolution of the expansion plume.

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