Abstract
Interplanetary dust particles (IDPs) collected from the stratosphere are derived from asteroids and comets. The chondritic porous (CP) subset of IDPs, some of which are almost certainly cometary, are physically, chemically, and isotopically primitive objects. Large D/H and 15N isotopic anomalies provide evidence for survival of presolar interstellar components. Embedded silicate grains exhibit both crystallographic and trace element evidence of formation by (nebular) gas phase condensation. The fine-grained matrices of CP IDPs contain GEMS, submicrometer spheroids whose exotic properties resemble those of interstellar “amorphous silicate” grains which are ubiquitous throughout interstellar space. Some GEMS are embedded in isotopically non-solar carbonaceous matrix (with 15N ∼ 25 – 40%) (Messenger et al., 1996), providing a further hint of their presolar origins. It is possible, but as yet unproven, that some CP IDPs are composed exclusively of aggregates of inters tellar and circumstellar dust grains, and that they carry a detailed record of fundamental grain formation and destruction processes in space.
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Bradley, J.P. (1999). Interstellar Dust — Evidence from Interplanetar Dust Particles. In: Greenberg, J.M., Li, A. (eds) Formation and Evolution of Solids in Space. NATO ASI Series, vol 523. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4806-1_28
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DOI: https://doi.org/10.1007/978-94-011-4806-1_28
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