JPL Technical Report Server

Dynamical evolution of dust particles in the Kuiper disk

Show simple item record

dc.contributor.author Holmes, E. K. en_US
dc.contributor.author Dermot, S. F. en_US
dc.contributor.author Gustafson, B. en_US
dc.date.accessioned 2004-09-17T07:08:37Z
dc.date.available 2004-09-17T07:08:37Z
dc.date.issued 2002-07-29 en_US
dc.identifier.citation ESA Special Publication Series: Asteroids, Comets, Meteors en_US
dc.identifier.citation Berlin, Germany en_US
dc.identifier.clearanceno 02-1867 en_US
dc.identifier.uri http://hdl.handle.net/2014/9703
dc.description.abstract A Kuiper belt dust disk will have a resonant structure, arising because the Plutinos are in the 3:2 mean motion resonance with Neptune. We run numerical integrations of particles originating from Plutinos to determine what percentage of particles remain in the resonance for a variety of particle and source body sizes. The dynamical evolution of the particles is followed from source to sink with Poynting-Robertson light drag, solar wind drag, radiation pressure, the Lorentz force, neutral interstellar gas drag, and the effects of planetary gravitational perturbations included. The number of particles in the 3:2 resonance increases with decreasing p for the cases where the initial source bodies are small and the percentage of particles in resonance is not significantly changed by either the addition of the Lorentz force, as long as the potential of the particles is small (U = 5 V), or the effect of neutral interstellar gas drag. en_US
dc.format.extent 2798135 bytes
dc.format.mimetype application/pdf
dc.language.iso en_US
dc.subject.other Kuiper dust disk en_US
dc.title Dynamical evolution of dust particles in the Kuiper disk en_US


Files in this item

This item appears in the following Collection(s)

Show simple item record

Search


Browse

My Account