  In this study, we numerically investigated the orbital evolution of cometary
dust particles, with special consideration of the initial size frequency
distribution (SFD) and different evolutionary tracks according to initial orbit
and particle shape. We found that close encounters with planets (mostly
Jupiter) are the dominating factor determining the orbital evolution of dust
particles. Therefore, the lifetimes of cometary dust particles (~250 thousand
years) are shorter than the Poynting-Robertson lifetime, and only a small
fraction of large cometary dust particles can be transferred into orbits with
small values of a. The exceptions are dust particles from 2P/Encke and,
potentially, active asteroids that have little interaction with Jupiter. We
also found that the effect of dust shape, mass density, and SFD were not
critical in the total mass supply rate to the Interplanetary Dust Particle
(IDP) cloud complex when these quantities are confined by observations of
zodiacal light brightness and SFD around the Earth's orbit. When we incorporate
a population of fluffy aggregates discovered in the Earth's stratosphere and
the coma of 67P/Churyumov-Gerasimenko within the initial ejection, the initial
SFD measured at the comae of comets (67P and 81P/Wild 2) can produce the
observed SFD around the Earth's orbit. Considering the above effects, we
derived the probability of mutual collisions among dust particles within the
IDP cloud for the first time in a direct manner via numerical simulation and
concluded that mutual collisions are mostly ignorable.
