scholarly journals Physical and Mineralogical Properties of Anhydrous Interplanetary Dust Particles in the Analytical Electron Microscope

1991 ◽  
Vol 126 ◽  
pp. 63-70
Author(s):  
J. P. Bradley
Keyword(s):  
Carbonaceous Material ◽  
Interplanetary Dust ◽  
Coarse Grained ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Electron Microscopic ◽  
Atmospheric Entry ◽  
Fine Grained ◽  
Microscopic Studies ◽  
Solar Flare Tracks

AbstractThe fine grained mineralogy and petrography of anhydrous “pyroxene” and “olivine” classes of chondritic interplanetary dust have been investigated by numerous electron microscopic studies. The “pyroxene” interplanetary dust particles (IDPs) are porous, unequilibrated assemblages of mineral grains, metal, glass, and carbonaceous material. They contain enstatite whiskers, FeNi carbides, and high-Mn olivines and pyroxenes, all of which are likely to be well preserved products of nebular gas reactions. Solar flare tracks are prominent in most “pyroxene” IDPs, indicating that they were not strongly heated during atmospheric entry. The “olivine” IDPs are coarse grained, equilibrated mineral assemblages that have probably experienced strong heating. Since most “olivine” IDPs do not contain tracks, it is possible that this heating occurred during atmospheric entry.

scholarly journals Interstellar and Solar System organic matter preserved in interplanetary dust

2015 ◽  
Vol 11 (A29B) ◽  
pp. 426-426
Author(s):  
Scott Messenger ◽  
K. Nakamura-Messenger
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Carbonaceous Material ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Fine Grained ◽  
Mass Fractionation ◽  
Current State ◽  
Short Period

AbstractInterplanetary dust particles (IDPs) collected in the Earths stratosphere derive from collisions among asteroids and by the disruption and outgassing of short-period comets. Chondritic porous (CP) IDPs are among the most primitive Solar System materials. CP-IDPs have been linked to cometary parent bodies by their mineralogy, textures, C-content, and dynamical histories. CP-IDPs are fragile, fine-grained (< um) assemblages of anhydrous amorphous and crystalline silicates, oxides and sulfides bound together by abundant carbonaceous material. Ancient silicate, oxide, and SiC stardust grains exhibiting highly anomalous isotopic compositions are abundant in CP-IDPs, constituting 0.01-1% of the mass of the particles. The organic matter in CP-IDPs is isotopically anomalous, with enrichments in D/H reaching 50x the terrestrial SMOW value and 15N/14N ratios up to 3x terrestrial standard compositions. These anomalies are indicative of low T (10-100 K) mass fractionation in cold molecular cloud or the outermost reaches of the protosolar disk. The organic matter shows distinct morphologies, including sub-um globules, bubbly textures, featureless, and with mineral inclusions. Infrared spectroscopy and mass spectrometry studies of organic matter in IDPs reveals diverse species including aliphatic and aromatic compounds. The organic matter with the highest isotopic anomalies appears to be richer in aliphatic compounds. These materials also bear similarities and differences with primitive, isotopically anomalous organic matter in carbonaceous chondrite meteorites. The diversity of the organic chemistry, morphology, and isotopic properties in IDPs and meteorites reflects variable preservation of interstellar/primordial components and Solar System processing. One unifying feature is the presence of sub-um isotopically anomalous organic globules among all primitive materials, including IDPs, meteorites, and comet Wild-2 samples returned by the Stardust mission. We will present an overview of the current state of understanding of the properties and origins of organic matter in primitive IDPs.

scholarly journals Cometary dust in Antarctic micrometeorites

2012 ◽  
Vol 8 (S288) ◽  
pp. 123-129 ◽  
Author(s):  
Naoya Imae
Keyword(s):  
Interstellar Dust ◽  
Compositional Analysis ◽  
Interplanetary Dust ◽  
Coarse Grained ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Interstellar Gas ◽  
Cometary Nuclei ◽  
Fine Grained ◽  
Cometary Dust

AbstractCometary nuclei consist of aggregates of interstellar dust particles less than ~1 μm in diameter and can produce rocky dust particles as a result of the sublimation of ice as comets enter the inner solar system. Samples of fine-grained particles known as chondritic porous interplanetary dust particles (CP-IDPs), possibly from comets, have been collected from the Earth's stratosphere. Owing to their fine-grained texture, these particles were previously thought to be condensates formed directly from interstellar gas. However, coarse-grained chondrule-like objects have recently been observed in samples from comet 81P/Wild 2. The chondrule-like objects are chemically distinct from chondrules in meteoritic chondrites, possessing higher MnO contents (0.5 wt%) in olivine and low-Ca pyroxene. In this study, we analyzed AMM samples by secondary electron microscopy and backscattered electron images for textural observations and compositional analysis. We identified thirteen AMMs with characteristics similar to those of the 81P/Wild 2 samples, and believe that recognition of these similarities necessitates reassessment of the existing models of chondrule formation.

scholarly journals The Question of Presolar Components within Interplanetary Dust Particles (IDPs) Collected in the Stratosphere

2002 ◽  
Vol 12 ◽  
pp. 34-37 ◽  
Author(s):  
John P. Bradley
Keyword(s):  
Solar Nebula ◽  
Carbonaceous Material ◽  
Building Blocks ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Space Observatory ◽  
Interplanetary Dust Particles ◽  
Infrared Space Observatory ◽  
Fine Grained ◽  
Astronomical Dust

AbstractInterplanetary dust particles (IDPs) are from asteroids and comets, and they are the smallest and most fine-grained meteoritic objects available for laboratory investigation. Cometary IDPs are of special significance because they are presently the only samples of comets, and comets are expected to be enriched in preserved solar nebula and presolar components. These components may include not only cosmically rare refractory circumstellar grains(e.g. SiC) that are recovered from meteorites but also cosmically abundant interstellar silicates and carbonaceous grains that were the fundamental building blocks of the Solar System. D/H ratios measured in IDPs are consistent with the survival of interstellar carbonaceous material, and some IDPs contain glassy grains with properties similar to those of interstellar “amorphous silicates”. Submicrometer forsterite and enstatite crystals in IDPs resemble circumstellar silicates detected by the Infrared Space Observatory (ISO). ISO also detected a broad ~ 23 µm feature around several stars, and a similar feature observed in IDP spectra is due to submicrometer FeNi sulfide grains, suggesting that sulfide grains may be a significant constituent of astronomical dust.

scholarly journals Constraints on the Parent Bodies of Collected Interplanetary Dust Particles

1991 ◽  
Vol 126 ◽  
pp. 397-404 ◽  
Author(s):  
S. A. Sandford
Keyword(s):  
Infrared Spectra ◽  
Deep Sea ◽  
Interplanetary Dust ◽  
Parent Body ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Atmospheric Entry ◽  
Silicate Minerals ◽  
Ice Caps ◽  
Entry Models

AbstractSamples of interplanetary dust particles (IDPs) have now been collected from the stratosphere, from the Earth’s ocean beds, and from the ice caps of Greenland and Antarctica The most likely candidates for the sources of these particles are comets and asteroids. Comparison of the infrared spectra, elemental compositions, and mineralogy of the collected dust with atmospheric entry models and data obtained from cometary probes and telescopic observations has provided important constraints on the possible sources of the various types of collected dust. These constraints lead to the following conclusions. First, most of the deep sea, Greenland, and Antarctic spherules larger than 100 μm are derived from asteroids. Second, the stratospheric IDPs dominated by hydrated layer-lattice silicate minerals are also most likely derived from asteroids. Finally, the stratospheric IDPs dominated by the anhydrous minerals olivine and pyroxene are most likely from comets. The consequences of these parent body assignments are discussed.

scholarly journals The effects of atmospheric entry heating on organic matter in interplanetary dust particles and micrometeorites

2020 ◽  
Vol 540 ◽  
pp. 116266 ◽  
Author(s):  
M.E.I. Riebe ◽  
D.I. Foustoukos ◽  
C.M.O'D. Alexander ◽  
A. Steele ◽  
G.D. Cody ◽  
...  
Keyword(s):  
Organic Matter ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Atmospheric Entry

scholarly journals A Comprehensive Study of Major, Minor, and Light Element Abundances in Over 100 Interplanetary Dust Particles

1996 ◽  
Vol 150 ◽  
pp. 283-286 ◽  
Author(s):  
Kathie L. Thomas ◽  
Lindsay P. Keller ◽  
David S. McKay
Keyword(s):  
Major Element ◽  
Light Element ◽  
Carbonaceous Material ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Element Abundances ◽  
Rich Material ◽  
Individual Grains ◽  
Comprehensive Study

AbstractOver 100 individual and cluster interplanetary dust particles (IDPs) have been analyzed for bulk abundances of 15 elements (C, O, Na, Mg, Al, Si, P, S, K, Ca, Ti, Cr, Mn, Fe, Ni). In general, IDPs have chondritic major element abundances, within a factor of 2 of the CI chondrites, and have carbon contents which average ~2-3 times higher than that of the most primitive, carbon-rich, carbonaceous meteorites (CI). The C-rich material is largely amorphous and is distributed throughout the particle as a matrix surrounding individual grains. The carbonaceous material has either smooth or vesicular texture; the latter texture suggests that volatiles could have been lost by particle heating which occurs during entry through the Earth's atmosphere.

Complementary Laboratory Measurements of Individual Interplanetary Dust Particles

1985 ◽  
Vol 85 ◽  
pp. 149-155
Author(s):  
A. Fahey ◽  
K.D. McKeegan ◽  
S.A. Sandford ◽  
R.M. Walker ◽  
B. Wopenka ◽  
...  
Keyword(s):  
Ir Spectra ◽  
Secondary Ion Mass Spectrometry ◽  
Molecular Spectroscopy ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Infrared Transmission ◽  
Interplanetary Dust Particles ◽  
Secondary Ion ◽  
Complementary Analysis ◽  
Solar Flare Tracks

AbstractComplementary analysis techniques including electron microscopy (SEM/EDX and TEM), molecular spectroscopy (FTIR and Raman), and secondary ion mass spectrometry (SIMS), are used to study individual dust particles collected in the stratosphere. Large deuterium enrichments and solar flare tracks show that most particles in the “chondritic” class are interplanetary dust particles (IDPs). Infrared transmission spectra of most IDPs fall into three major classes (layer-lattice silicates, pyroxenes and olivines). TEM and Raman measurements confirm this classification. The IR spectra show certain similarities to spectra observed in comets and protostars. In particular the 6.8 μm features observed in protostars and IDPs may have a common origin. Large D excesses are observed in IDPs of the first two IR classes. The correlation of D/H ratios with the C concentration indicates a carbonaceous carrier of the excess D. The D enrichments and IR spectra provide links to interstellar molecular cloud material.

scholarly journals Carbonaceous Material in Extra-terrestrial Matter

2015 ◽  
Vol 11 (A29A) ◽  
pp. 257-260
Author(s):  
Zita Martins
Keyword(s):  
Amino Acids ◽  
Carbonaceous Material ◽  
Interplanetary Dust ◽  
Hypervelocity Impact ◽  
Dust Particles ◽  
Early Earth ◽  
Carbonaceous Chondrites ◽  
Interplanetary Dust Particles ◽  
Living Organisms ◽  
Impact Shock

AbstractComets, asteroids, meteorites, micrometeorites, interplanetary dust particles (IDPs), and ultra-carbonaceous Antarctic micrometeorites (UCAMMs) may contain carbonaceous material, which was exogenously delivered to the early Earth. Carbonaceous chondrites have an enormous variety of extra-terrestrial compounds, including all the key compounds important in terrestrial biochemistry. Comets contain several carbon-rich species and, in addition, the hypervelocity impact-shock of a comet can produce several α-amino acids. The analysis of the carbonaceous content of extra-terrestrial matter provides a window into the resources delivered to the early Earth, which may have been used by the first living organisms.

scholarly journals Comets, Meteorites and Interplanetary Dust

1989 ◽  
Vol 8 ◽  
pp. 281-286
Author(s):  
D. E. Brownlee
Keyword(s):  
Interplanetary Dust ◽  
Dust Particles ◽  
Substantial Fraction ◽  
Interplanetary Dust Particles ◽  
Atmospheric Entry ◽  
Presolar Grains ◽  
Carbon And Nitrogen ◽  
The Earth ◽  
Cometary Material ◽  
Insight Into

AbstractCometary debris of all sizes impacts the Earth but it is likely that only particles the size of dust survive atmospheric entry and are collected as meteoritic samples. Conventional meteorites and a substantial fraction of collected interplanetary dust particles appear to be asteroidal debris. Nearly half of the collected interplanetary particles have properties consistent with cometary material and resemble Halley dust that has lost the maiority of its carbon and nitrogen. These particles might be aggregates of presolar grains ana they provide some insight into the properties of interstellar grains.

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