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In this study, we numerically investigated the orbital evolution of cometarydust particles, with special consideration of the initial size frequencydistribution (SFD) and different evolutionary tracks according to initial orbitand particle shape. We found that close encounters with planets (mostlyJupiter) are the dominating factor determining the orbital evolution of dustparticles. Therefore, the lifetimes of cometary dust particles (~250 thousandyears) are shorter than the Poynting-Robertson lifetime, and only a smallfraction of large cometary dust particles can be transferred into orbits withsmall values of a. The exceptions are dust particles from 2P/Encke and,potentially, active asteroids that have little interaction with Jupiter. Wealso found that the effect of dust shape, mass density, and SFD were notcritical in the total mass supply rate to the Interplanetary Dust Particle(IDP) cloud complex when these quantities are confined by observations ofzodiacal light brightness and SFD around the Earth's orbit. When we incorporatea population of fluffy aggregates discovered in the Earth's stratosphere andthe coma of 67P/Churyumov-Gerasimenko within the initial ejection, the initialSFD measured at the comae of comets (67P and 81P/Wild 2) can produce theobserved SFD around the Earth's orbit. Considering the above effects, wederived the probability of mutual collisions among dust particles within theIDP cloud for the first time in a direct manner via numerical simulation andconcluded that mutual collisions are mostly ignorable.

Evolution of Cometary Dust Particles to the Orbit of the Earth: Particle Size, Shape, and Mutual Collisions