Grain size distributions of Magneli phases and metallic titanium in chondritic porous interplanetary dust particles
Rietmeijer, Frans J.M. & Mackinnon, Ian D.R. (1989) Grain size distributions of Magneli phases and metallic titanium in chondritic porous interplanetary dust particles. In Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX, pp. 902-903.
A mineralogical survey of chondritic interplanetary dust particles (IDPs)showed that these micrometeorites differ significantly in form and texture from components of carbonaceous chondrites and contain some mineral assemblages which do not occur in any meteorite class1. Models of chondritic IDP mineral evolution generally ignore the typical (ultra-) fine grain size of consituent minerals which range between 0.002-0.1µm in size2. The chondritic porous (CP) subset of chondritic IDPs is probably debris from short period comets although evidence for a cometary origin is still circumstantial3. If CP IDPs represent dust from regions of the Solar System in which comet accretion occurred, it can be argued that pervasive mineralogical evolution of IDP dust has been arrested due to cryogenic storage in comet nuclei. Thus, preservation in CP IDPs of "unusual meteorite minerals", such as oxides of tin, bismuth and titanium4, should not be dismissed casually. These minerals may contain specific information about processes that occurred in regions of the solar nebula, and early Solar System, which spawned the IDP parent bodies such as comets and C, P and D asteroids6. It is not fully appreciated that the apparent disparity between the mineralogy of CP IDPs and carbonaceous chondrite matrix may also be caused by the choice of electron-beam techniques with different analytical resolution. For example, Mg-Si-Fe distributions of Cl matrix obtained by "defocussed beam" microprobe analyses are displaced towards lower Fe-values when using analytical electron microscope (AEM)data which resolve individual mineral grains of various layer silicates and magnetite in the same matrix6,7. In general, "unusual meteorite minerals" in chondritic IDPs, such as metallic titanium, Tin01-n(Magneli phases) and anatase8 add to the mineral data base of fine-grained Solar System materials and provide constraints on processes that occurred in the early Solar System.
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|Item Type:||Conference Paper|
|Additional Information:||GeoRef, Copyright 2009, American Geological Institute.
|Keywords:||accretion, carbonaceous chondrites, chondrites, comets, composition, distribution, fabric, genesis, grain size, grains, interplanetary dust, interplanetary space, metals, meteorites, meteoroids, parent materials, porous materials, solar nebula, solar system, stony meteorites, textures, titanium|
|Subjects:||Australian and New Zealand Standard Research Classification > EARTH SCIENCES (040000) > GEOLOGY (040300) > Extraterrestrial Geology (040302)
Australian and New Zealand Standard Research Classification > EARTH SCIENCES (040000) > GEOLOGY (040300) > Mineralogy and Crystallography (040306)
|Divisions:||Current > Institutes > Institute for Future Environments|
|Copyright Owner:||Copyright 1989 (please consult the authors).|
|Deposited On:||21 Jan 2013 06:30|
|Last Modified:||04 Apr 2013 16:09|
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