Collisional evolution and the resulting mass distribution of interplanetary dust

Details Collisional evolution and the resulting mass distribution of interplanetary dust Collisional evolution and the resulting mass distribution of interplanetary dust

Jun 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998ep%26s...50..521i&link_type=abstract

Earth, Planets and Space, Volume 50, p. 521-529.

Physics

7

Scientific paper

On the basis of numerical approaches for the collisional and orbital evolution of dust particles, the number density distribution of interplanetary dust with the mass range of m≥ 10-12 g is investigated. The slope of the mass distribution of dust particles strongly depends on the radial dependence of dust production by their parent bodies, and the collisional interaction between particles. Specifically, the m-7/3dependence of the number density distribution at 1AU for m≥10-6g can be explained through the balance between the collisional loss of particles and the dust supply, whereas the m-4/3dependence for 10-12g ≤ m≤10-6g particles is derived from simple Poynting-Robertson orbital decay. A possible model of the dust populations of asteroidal, cometary, and Edgeworth-Kuiper belt origin that is consistent with the observed dust flux at a solar distance of 1AU is presented.

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