Computer Science
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002phdt.........6n&link_type=abstract
Thesis (PhD). BAYLOR UNIVERSITY, Source DAI-B 63/06, p. 2875, Dec 2002, 160 pages.
Computer Science
1
Scientific paper
Dust particles are ubiquitous in the solar system, residing at both its outer limits and its innermost regions. These dust particles are subjected to a variety of forces and environments and have been studied and reported in the literature for over thirty years. This study expands on previous numerical studies by incorporating more realistic magnetic fields and charging mechanisms while also taking into account the proper motion of the system's main bodies (the planets Neptune and Mars and the asteroid Ceres) around the Sun. The specific forces acting on individual dust grains are calculated within each region of interest and include the gravitational forces, the radiation pressure force, the Poynting-Robertson effect, and electromagnetic forces. Specifically, dust particles ejected from the moons of Mars were examined to determine grain orbital longevity as well as possible contributions to a hypothesized dust torus encircling the planet. The grains were found to exist in a torus-structure influenced by the interplanetary magnetic field. Dust ejected from the inner three moons of Neptune was also examined to determine possible contributions to the planet's ring structure as well as grain lifetimes, spatial distributions, and structural formation characteristics. This dust was found to attain the same orbital parameters as two of the rings (rings 1989N3R and 1989N2R) after only ten years. Dust particles ejected from the surface of the asteroid Ceres were examined to determine overall grain lifetimes and orbital trajectories. It was determined that the angle at which grains were ejected greatly influenced their fate. The possibility of the formation of a ring type structure around Ceres was investigated as well. Particles greater than 40 μm in radius were found to survive after the addition of a magnetic field as compared to the finding that only particles greater than 100 μm survive without the magnetic field. Finally, a solar system dust ring was modeled to determine its overall fate and determine temporal zones of enhanced and depleted dust densities. This data was compared with the fording that the addition of multiple planets created dust zones of concentration due to their gravitational interactions.
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