Earth Planets Space, Vol. 50 (Nos. 6, 7), pp. 521-529, 1998
The Graduate School of Science and Technology, Kobe University, Nada, Kobe 657-8501, Japan
(Received October 8, 1997; Revised March 3, 1998; Accepted March 13, 1998)
Abstract: 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 m10-6g can be explained through the balance between the collisional loss of particles and the dust supply, whereas the m-4/3dependence for 10-12g m10-6g 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.