Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mmsai..73..684k&link_type=abstract
in Memorie della Società' Astronomica Italiana, vol. 73, no. 3, p. 684
Astronomy and Astrophysics
Astronomy
2
Scientific paper
Dust particles originating in the main asteroid belt encounter both mean motion and secular resonances as they spiral in towards the Sun under the effects of Poynting-Robertson (P-R) light drag and solar-wind drag. This numerical investigation has shown that the dynamical behaviour of large asteroidal dust particles, greater than about 100 microns in diameter, originating from the Eos family is significantly different to that exhibited by smaller asteroidal particles from the same source. In particular, passage through the ?6 and ?16 secular resonances at the inner edge of the main asteroid belt had a pronounced effect on the large dust particles that was not observed in the case of the small particles. In some examples, the large asteroidal dust particles evolved onto almost comet-like orbits with moderate to high eccentricities and inclinations. This contrasting behaviour arises because the large dust particles evolve through the secular resonances relatively slowly in comparison to the small particles, due to the weaker action of P-R light drag and solar-wind drag on the large particles, and hence allow more time for the secular resonances to act. Temporary trapping of the large dust particles in mean motion resonances (MMRs) with Jupiter is also more common, especially trapping in the 5:2 and 3:1 interior jovian MMRs located in the main asteroid belt. These results have important implications for the structure of the zodiacal cloud and the origins and size-frequency distributions of interplanetary dust particles accreted by the Earth.
Dermott Stanley F.
Grogan Keith
Kehoe Thomas J. J.
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