Abstract
Recently released cometary particles are most likely aggregates of core-mantle building blocks. Their structures are therefore porous (fluffy particles). Lunar Microcrater studies and in situ dust experiments have shown that the majority of the interplanetary dust particles are compact grains with densities between 3 and 8 g/cm3, although ~ 20% of the interplanetary dust is of low density (<1 g/cm3). Under the assumption that cometary grains slowly lose their mantle material, the grains become denser. Simultaneously the orbits also become more circular as compared to the original cometary orbit. This has been observed by the Helios dust experiment
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Fechtig, H., Mukai, T. (1985). Dust of Variable Porosities (Densities) in the Solar System. In: Klinger, J., Benest, D., Dollfus, A., Smoluchowski, R. (eds) Ices in the Solar System. NATO ASI Series, vol 156. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5418-2_16
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DOI: https://doi.org/10.1007/978-94-009-5418-2_16
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