Dust grain orbital behavior around Mars

Details Dust grain orbital behavior around Mars Dust grain orbital behavior around Mars

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28.1005n&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 005.

Computer Science

Interplanetary Dust, Mars Atmosphere, Particle Motion, Orbits, Gravitational Fields, Runge-Kutta Method

Scientific paper

The orbital motion of dust grains in the Mars system has recently become a well-studied phenomena due to in situ data from expeditions to the planet. One possible dust grain source in the Mars system is ejecta caused by impacts of cm to micron size particles on the Martian moons, Phobos and Deimos. Impacts from particles larger than micron size eject dust grain clouds having both a size and velocity distribution which is not yet well known. This study tracks the orbits of such ejecta, assuming each particle to initially have a random velocity. It is shown that such velocities result in highly complicated dust particle motion, several aspects of which are examined.

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