Modeling the particle mass distribution within 1 AU of the Sun

We propose a method for estimating the particle flux and number density distribution of interplanetary dust particles within 1 AU of the Sun. The method takes into account both the evolution of dust particles by collision and Poynting–Robertson orbital decay. The collisional evolution and the resulting particle mass distribution function both depend strongly on the orbits of collision fragments. Our preliminary results indicate that the flux of hyperbolic particles (β-meteoroids) with masses in the range 10−15 < m < 10−13 g at 1 AU will directly lead to the supply of m ⩾ 10−7 g particles inside 1 AU. Moreover, we show that the slope of the particle mass distribution function inside 1 AU may differ significantly from that at 1 AU if we assume that the flux distribution inside 1 AU does not vary with time.