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 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 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 Dome C ultracarbonaceous Antarctic micrometeorites

2018 ◽  
Vol 609 ◽  
pp. A65 ◽  
Author(s):  
E. Dartois ◽  
C. Engrand ◽  
J. Duprat ◽  
M. Godard ◽  
E. Charon ◽  
...  
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Absorption Band ◽  
Raman Spectra ◽  
Interplanetary Dust ◽  
Organic Component ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Lower Oxygen ◽  
Carbonyl Absorption Band

Context. UltraCarbonaceous Antarctic MicroMeteorites (UCAMMs) represent a small fraction of interplanetary dust particles reaching the Earth’s surface and contain large amounts of an organic component not found elsewhere. They are most probably sampling a contribution from the outer regions of the solar system to the local interplanetary dust particle (IDP) flux. Aims. We characterize UCAMMs composition focusing on the organic matter, and compare the results to the insoluble organic matter (IOM) from primitive meteorites, IDPs, and the Earth. Methods. We acquired synchrotron infrared microspectroscopy (μFTIR) and μRaman spectra of eight UCAMMs from the Concordia/CSNSM collection, as well as N/C atomic ratios determined with an electron microprobe. Results. The spectra are dominated by an organic component with a low aliphatic CH versus aromatic C=C ratio, and a higher nitrogen fraction and lower oxygen fraction compared to carbonaceous chondrites and IDPs. The UCAMMs carbonyl absorption band is in agreement with a ketone or aldehyde functional group. Some of the IR and Raman spectra show a C≡N band corresponding to a nitrile. The absorption band profile from 1400 to 1100 cm-1 is compatible with the presence of C-N bondings in the carbonaceous network, and is spectrally different from that reported in meteorite IOM. We confirm that the silicate-to-carbon content in UCAMMs is well below that reported in IDPs and meteorites. Together with the high nitrogen abundance relative to carbon building the organic matter matrix, the most likely scenario for the formation of UCAMMs occurs via physicochemical mechanisms taking place in a cold nitrogen rich environment, like the surface of icy parent bodies in the outer solar system. The composition of UCAMMs provides an additional hint of the presence of a heliocentric positive gradient in the C/Si and N/C abundance ratios in the solar system protoplanetary disc evolution.

scholarly journals Presolar grains in the Solar System: Connections to stellar and interstellar organics

2008 ◽  
Vol 4 (S251) ◽  
pp. 343-344
Author(s):  
Larry R. Nittler
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Interplanetary Dust ◽  
Asymptotic Giant Branch ◽  
Dust Particles ◽  
Interplanetary Dust Particles ◽  
Molecular Chemistry ◽  
Stellar Outflows ◽  
Isotopic Compositions ◽  
Polycyclic Aromatic

AbstractA small fraction of primitive meteorites and interplanetary dust particles (IDPs) consists of grains of presolar stardust. These grains have extremely unusual isotopic compositions, relative to all other planetary materials, indicating that they condensed in the outflows and explosions of prior generations of stars (Clayton & Nittler 2004). Identified presolar grain types include silicate, oxide and carbonaceous phases. The latter include graphitic carbon, diamond and SiC. Although many of these phases do not have a direct connection to organic chemistry, this is not true of the graphitic spherules. Many of these, with isotopic compositions indicating an origin in C-rich asymptotic giant branch (AGB) star outflows, have a structure consisting of naonocrystalline cores surrounded by well-graphitized C (Bernatowicz et al. 1996). The cores include isotopically anomalous polycyclic aromatic hydrocarbons (Messenger et al. 1998) and represent a link between molecular chemistry and dust condensation in stellar outflows. Meteorites and IDPs also contain abundant isotopically anomalous organic matter, including distinct organic grains, some of which probably formed in stellar outflows and/or the interstellar medium (ISM) (Busemann et al. 2006, Floss et al. 2004). In some IDPs, deuterium- and 15N-enriched organic matter is closely associated with presolar silicate grains (Messenger et al. 2005, Nguyen et al. 2007), suggesting an association in the ISM prior to Solar System formation.

The origin of organic matter in the solar system: evidence from the interplanetary dust particles

2003 ◽  
Vol 67 (24) ◽  
pp. 4791-4806 ◽  
Author(s):  
G.J Flynn ◽  
L.P Keller ◽  
M Feser ◽  
S Wirick ◽  
C Jacobsen
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Interplanetary Dust Particles

scholarly journals The Origin of Organic Matter in the Solar System: Evidence from the Interplanetary Dust Particles

2004 ◽  
Vol 213 ◽  
pp. 275-280 ◽  
Author(s):  
G. J. Flynn ◽  
L. P. Keller ◽  
C. Jacobsen ◽  
S. Wirick
Keyword(s):  
Organic Matter ◽  
Gas Phase ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Aqueous Processing ◽  
Interplanetary Dust Particles ◽  
Volatile Elements ◽  
Edge Structure ◽  
X Ray ◽  
X Ray Absorption

Interplanetary dust particles (IDPs), ∼ 10μm particles from comets and asteroids, have been collected by NASA from the Earth's stratosphere. We compared carbon X-ray Absorption Near-Edge Structure (XANES) and Fourier Transform Infra-Red (FTIR) spectra of anhydrous and hydrated interplanetary dust particles and found that anhydrous and hydrated IDPs have similar types and abundances of organic carbon. This is different from results on meteorites, which show that hydrated carbonaceous meteorites contain abundant organic matter, while anhydrous carbonaceous meteorites contain less carbon mostly in elemental form. But all anhydrous carbonaceous meteorites are depleted in moderately volatile and volatile elements in a pattern that suggested they experienced temperatures in excess of 1200°C, a temperature sufficient to destroy any organic matter they originally contained, while many anhydrous IDPs show no evidence of severe heating. These IDP results indicate that the bulk of the pre-biotic organic matter in extraterrestrial materials formed before aqueous processing, possibly by irradiation of C-bearing ices or by a Fisher-Tropsch type process operating in the gas phase of the nebula or in the interstellar medium.

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.

scholarly journals A Common Origin for Organics in Meteorites and Comets: Was It Interstellar?

2011 ◽  
Vol 7 (S280) ◽  
pp. 288-301 ◽  
Author(s):  
Conel M. O'D. Alexander
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Organic Material ◽  
Protoplanetary Disks ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Soluble Organic Matter ◽  
Interplanetary Dust Particles ◽  
Cold Environments ◽  
Insoluble Material

AbstractThe insoluble organic material preserved in primitive chondritic meteorites shares many similarities with the refractory organic material in interplanetary dust particles and comets, suggesting that there is a genetic link between the organic matter in objects that formed between ~3 AU and ~30 AU from the Sun. These similarities include large D and 15N enrichments in bulk and even more extreme enrichments in isotopic hotspots. The enrichments attest to formation in very cold environments, either in the outer Solar System or the protosolar molecular cloud. There are many properties of this organic material that are consistent with an interstellar origin, but a Solar System origin cannot be ruled out. Similar organic material is presumably an important component of most protoplanetary disks, and heating or sputtering of this material would be a source of PAHs in disks. The soluble organic matter was more heavily effected by processes on the chondritic parent bodies than the insoluble material. Amino acids, for instance, probably formed by reaction of ketones and aldehydes with NH3 and HCN. The accretion of the relatively volatile NH3 and HCN, presumably in ices, strengthens the chondrite-comet connection. However, unlike most comets the water in chondrites, when it was accreted, had D/H ratios that were similar to or depleted relative to Earth.

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