Meteoroid size3/28/2023 First the flux to a Randomly Tumbling Plate (RTP) is predicted for a mass range of 10 −15–1 g. The different meteoroid models are compared for LEO (400 km circular or bit and 51.6 inclination) and Geostationary orbit (GEO). ![]() The ISD population was adopted from the Divine-Staubach model, with a re-normalisation to take additional ULYSSES dust detector data into account. ![]() 2005a, b, c), an attempt was made to construct a meteoroid model, based on the physical effects that influence meteoroid orbit and sources, in addition to fitting model predictions to observations. With the IMEM/Dikarev model (Dikarev et al. Solar radiation pressure was added as a second perturbation force and an additional population, Inter Stellar Dust (ISD), was implemented. 1997) upgraded Divine’s model using new data from GALILEO and ULYSSES dust detectors. The model is based on five different populations each having separable distributions in particle mass, inclination, eccentricity, and perihelion distance. The Divine interplanetary model (Divine 1993) was one of the first models with non-isotropic distributions. Taylor used data from the Harvard Radio Meteor Project (HMRP) to develop a velocity distribution, which is valid for near Earth orbits and the interplanetary space near 1 AU. Therefore, it is valid for Low Earth Orbits (LEO) only. SSP 30425 is a velocity distribution, developed for the International Space Station. 1994) or Taylor (Taylor 1995), to include directional effects. The Grün model is frequently used with added velocity distributions, such as from SSP 30425 (Kessler et al. For the conversion of crater sizes to particle masses, a constant velocity of 20 km/s was used. 1985) assumes an isotropic meteoroid distribution which is based on lunar crater, zodiacal light and in situ measurement data. The Grün interplanetary flux model (Grün et al. The persisting differences even for near Earth space can be seen as surprising in view of the numerous ground based (optical and radar) and in situ (captured Inter Stellar Dust Particles, in situ detectors and analysis of retrieved hardware) measurements and simulations. Main differences are presented and analysed. In this paper flux predictions by the various models to Earth orbiting spacecraft are compared. Examples are the velocity and directional distributions and the assumed meteoroid sources. However, in many respects these models differ considerably. They typically cover mass ranges from 10 −18 g to 1 g and are applicable for model specific Sun distance ranges between 0.1 AU and 20 AU Near 1 AU averaged fluxes (over direction and velocities) for all these models are tuned to the well established interplanetary model by Grün et al. These include the Divine-Staubach and the Dikarev model. Over the last decade several new models for the sporadic interplanetary meteoroid flux have been developed.
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