Infrared spectroscopy of interplanetary dust in the laboratory

Fraundorf, P.; Patel, Rahul; Freeman, John J.

doi:10.1016/0019-1035(81)90185-8

Cited by 15 publications

(5 citation statements)

References 22 publications

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“…The pervasiveness of these three basic types of chondritic particles was also confirmed for the JSC collection by Mackinnon et al [1982a]. Infrared (IR) spectroscopy of individual chondritic micrometeorites by Fraundorf et al [1981] and Sandford and Walker [1985] indicated that "hydrated" features at 3500 and 1650 cm -1 may provide convenient criteria for the classification of particles. These hydrated features are generally attributed to the presence of layer silicates in micrometeorites .…”

Section: Euhedral Single Crystals and Fragmentsmentioning

confidence: 78%

Mineralogy of chondritic interplanetary dust particles

Mackinnon¹,

Rietmeijer²

1987

Reviews of Geophysics

134

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From a mineralogical survey of approximately 30 chondritic micrometeorites collected from the lower stratosphere and studied in detail using current electron microscopy techniques, it is concluded that these particles represent a unique group of extraterrestrial materials. 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 class. Electron microscope investigations of chondritic micrometeorites have established that these materials (1) are extraterrestrial in origin, (2) existed in space as small objects, (3) endured minimal alteration by planetary processes since formation, and (4) can suffer minimal pulse heating (<600øC) on entering earth's atmosphere. The probable sources for chondritic interplanetary dust particles (IDPs) are cometary and asteroidal debris and, perhaps to a lesser extent, interstellar regions. These sources have not been conclusively linked to any specific mineralogical subset of IDP, although the chondritic porous (CP) aggregate is considered of likely cometary origin. Chondritic IDPs occur in two predominant mineral assemblages:(1) carbonaceous phases and phyllosilicates and (2) carbonaceous phases and nesosilicates or inosilicates, although particles with both types of silicate assemblages are observed. Olivines, pyroxenes, layer silicates, and carbon-rich phases are the most commonly occurring minerals in many chondritic IDPs. Other phases often observed in variable proportions include sulphides, spineIs, metals, metal carbides, carbonates, and minor amounts of sulphates and phosphates. Individual mineral grain sizes range from micrometers (primarily pyroxenes and olivines) to nanometers, with the predominant size for all phases less than 100 nm. Specific mineral characteristics for particular chondritic IDPs provide an indication of processes which may have occurred prior to collection in the earth's stratosphere. For example, pyroxene mineralogy in some chondritic aggregates is consistent with condensation from a vapor phase and, we consider, with condensation in a turbulent solar nebula at relatively low temperatures (<1000øC). Carbonaceous phases present in other CP aggregates have been used to imply low-temperature formation processes such as Fischer-Tropsch synthesis (-530øC) or carbonization and graphitization (--•315øC). Alteration processes have been implicated in the formation of some layer silicates in CP aggregates and may have involved hydrocryogenic alteration at <0øC. In general, interpretations of transformation processes on submicrometer-size minerals in chondritic IDPs are consistent with formation at a radius equivalent to the asteroid belt or greater during the later stages of solar nebula evolution using currently available models.

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Section: Euhedral Single Crystals and Fragmentsmentioning

confidence: 78%

Mineralogy of chondritic interplanetary dust particles

Mackinnon¹,

Rietmeijer²

1987

Reviews of Geophysics

134

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“…Fraundorf et al. () first reported the presence of carbon in IDPs by Raman measurements, and this work was followed up with more in‐depth Raman studies characterizing IDPs (Wopenka ; Quirico et al. ).…”

Section: Introductionmentioning

confidence: 99%

A Raman spectroscopic study of organic matter in interplanetary dust particles and meteorites using multiple wavelength laser excitation

Starkey

Franchi

Alexander

2013

Meteorit & Planetary Scien

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Abstract-Raman spectroscopy was used to investigate insoluble organic matter (IOM) from a range of chondritic meteorites, and a suite of interplanetary dust particles (IDPs). Three monochromatic excitation wavelengths (473 nm, 514 nm, 632 nm) were applied sequentially to assess variations in meteorite and IDP Raman peak parameters (carbon D and G bands) as a function of excitation wavelength (i.e., dispersion). Greatest dispersion occurs in CVs > OCs > CMs > CRs with type 3 chondrites compared at different excitation wavelengths displaying conformable relationships, in contrast to type 2 chondrites. These findings indicate homogeneity in the structural nature of type 3 chondrite IOM, while organic matter (OM) in type 2 chondrites appears to be inherently more heterogeneous. If type 2 and type 3 chondrite IOM shares a common source, then thermal metamorphism may have a homogenizing effect on the originally more heterogeneous OM. IDP Raman G bands fall on an extension of the trend displayed by chondrite IOM, with all IDPs having Raman parameters indicative of very disordered carbon, with almost no overlap with IOM.

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“…FTS spectra of Saturn have been used to study NH3 in both gaseous and solid form (28) in an attempt to understand its low abundance there. Remote mineralogical analysis of solid planetary, ring, satellite, and asteroid materials is a rich field, with detections of various ices in the outer solar system and of a number of mineralogical groups that correlate with known meteoritic materials (24,25,30,31,57,60). The only available IR spectrum of a comet was also obtained with an FTS (49).…”

Section: Solar and Stellar Studiesmentioning

confidence: 99%