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V. Dikarev, E. Grün (MPI fur Kernphysik), M. Landgraf (ESOC)
We construct a new meteoroid model that replaces the models by Divine (1993, {\em JGR} 98(E9), 17029--17048, ``Five population of interplanetary meteoroids'') and Staubach & Grün (1995, {\em Advances in Space Research} 16(11), 103--106, ``Development of an upgraded meteoroid model''). Our approach of describing the interplanetary dust cloud, however, is different from that of our predecessors. Instead of empirically found distribution functions, we use distributions that are determined by orbital evolution of various dust populations. The populations correspond to expected structures in zodiacal cloud. We determine the distributions of meteoroid-sized debris dispersed along the orbits of the parent bodies, comets and asteroids, meteoroids residing in the torus of debris scattered by Jupiter, and the distributions of small dust grains spiraling towards the Sun under the Poynting-Robertson drag from their parent bodies, including scattered meteoroids. The interstellar dust particles are represented by a physical model as well. Each distribution function has an arbitrary normalization factor corresponding to the unknown dust production rate for the population.
We use several data sets to validate the approach and to infer the population normalisation factors minimizing model residuals: interplanetary meteoroid size distribution observed at 1~AU, COBE DIRBE infrared observations, Galileo & Ulysses DDS in-situ impact counts, particle fluxes derived from the Helios~1 and Pioneer~10 and~11 dust experiments, and AMOR radar meteor survey.
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The author(s) of this abstract have provided an email address for comments about the abstract: dikarev@galileo.mpi-hd.mpg.de