Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p22c..02b&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #P22C-02
Physics
5199 General Or Miscellaneous, 6008 Composition, 6061 Remote Sensing, 6205 Asteroids And Meteoroids, 6210 Comets
Scientific paper
The atmospheric interactions of Leonid meteoroids are characterized by two sequential processes. First, incoming atmospheric molecules ablate the meteoroid surface and also interact with the ablated meteoroid-vapor molecules. Second, the ablated meteoroid molecules are deposited into the atmosphere and initiate an interaction leading to the observed meteor signature. To the authors knowledge, no one has developed an appropriate physically-based model of these, rarefied-flow, interaction processes. They cannot be adequately described even by the Navier-Stokes equations. Monte Carlo molecular simulations are used to separately describe the meteoroid ablation and the atmospheric response. The heat transfer and the drag coefficients are numerically calculated as a function of ablation rate. Most previous conservation equation models have assumed that these coefficients are constants. The Monte Carlo simulations indicate that their ratio can vary three orders of magnitude during an entry trajectory. Light curves have been calculated using the numerical results to describe the effects of ablation on the coefficients. These results are compared with those that assume constant coefficients. Monte Carlo molecular simulations of the nonequilibrium wake formation process have also been completed up to a level that includes dissociation effects. It is planned to next model the rarefied-flow ionization process. The results of this modeling will provide new insights concerning the transformation of the kinetic energy of meteoroid vapor molecules into observed radiative energy.
Baker Richard L.
Nelson Donald A.
Yee P. P.
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