A Numerical Study of Dust Distribution in the Atmosphere of Comet 67P/Churyumov-Gerasimenko

Details A Numerical Study of Dust Distribution in the Atmosphere of Comet 67P/Churyumov-Gerasimenko A Numerical Study of Dust Distribution in the Atmosphere of Comet 67P/Churyumov-Gerasimenko

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.2011z&link_type=abstract

American Astronomical Society, DPS meeting #41, #20.11

Astronomy and Astrophysics

Astronomy

Scientific paper

Success of Rosetta mission to Comet 67P/Churyumov-Gerasimenko (67P/C-G) requires development of dusty-gas coma model to assist in preparing the orbital strategy of the spacecraft, the delivery of the Philae surface module and the science operations.
We extended to 3D our Dust Monte-Carlo (DMC) simulation technique (Icarus, 2005, 176, 192-219) to study the dynamics of dust grains in the vicinity of three-dimensional shape of 67P/C-G derived by Lamy et al. (Space Sci. Rev., 2007, 128, 23). We assume that dust grains are spherical moving under influence of three forces: the nucleus gravitational force, gas coma aerodynamic force, and solar radiation pressure force, and consider the full mass range of ejectable grains. A multi-species gas model is based on gasdynamical solutions of Navier-Stokes equation combined with Boltzmann equation (BE-NSE) (Planet. Space Sci., 2002, 50, 983-1024) or kinetic solution based on the Direct Simulation Monte Carlo (DSMC) approach. The model was utilized to study the dusty coma of 67P/C-G over a range of probable conditions at the time of rendezvous with Rosetta spacecraft (rh 3 AU and Q 1026 - 1027 s-1).
The resulting complex grain motions are described in detail, as well as the resulting complex and often counter-intuitive dust coma structure. We discuss the implications of the dust flow for the evolution of the nucleus surface, and for the survival of a landing probe. Also we present comparison of results obtained by DMC and by the more efficient but less general Dust Multi-Fluid method.

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