Collisional evolution and the resulting mass distribution of interplanetary dust
© The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences. 1998
Received: 8 October 1997
Accepted: 13 March 1998
Published: 6 June 2014
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 ≥ 10−12g 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 −7/3 dependence of the number density distribution at 1 AU for m ≥ 10−6g can be explained through the balance between the collisional loss of particles and the dust supply, whereas the m −4/3 dependence 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 1 AU is presented.