Carbon abundance and silicate mineralogy of anhydrous interplanetary dust particles

Thomas, K. L.; Blanford, G. E.; Keller, L. P.; Klöck, W.; McKay, D. S.

doi:10.1016/0016-7037(93)90012-l

Cited by 161 publications

(127 citation statements)

References 26 publications

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“…First, their fine grained and fragile structure is consistent with properties of comets as inferred from the low strength of cometary meteors and the abundance of sub-m grains observed in cometary comae [66,67]. Second, CP-IDPs have C abundances that are more similar to comets than meteorites [51]. Third, CP-IDPs have high abundances of presolar grains and molecular cloud material [68][69][70].…”

Section: Constraints On Idp Source Bodiessupporting

confidence: 69%

See 1 more Smart Citation

Dust in the Solar System: Properties and Origins

Messenger¹,

Keller²,

Nguyen³

2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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Section: Constraints On Idp Source Bodiessupporting

confidence: 69%

“…The proportions of these phases are highly variable from particle to particle, and any one phase may dominate individual CP-IDPs. On average, the C abundance of CP-IDPs is 2-3x that of the Crich CI chondrite meteorites [51].…”

Section: Stratospheric Interplanetary Dust Particles (Idps)mentioning

confidence: 94%

Dust in the Solar System: Properties and Origins

Messenger¹,

Keller²,

Nguyen³

2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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“…OH bearing silicates have also been proposed to explain a band at ∼100 μm observed in emission in the spectrum of the young star HD 142527 (Malfait et al 1999). Interestingly, hydroxylated amorphous silicates are found within interplanetary dust particles (IDPs) in the GEMS (glass with embedded metal and sulphides; Thomas et al 1993;Bradley 1994;Bradley et al 2005). Some of these GEMS are believed to be presolar (Messenger et al 2003) and to originate from the ISM (Bradley et al 1999).…”

Section: Introductionmentioning

confidence: 99%

Hydroxyl radical production and storage in analogues of amorphous interstellar silicates: a possible “wet” accretion phase for inner telluric planets

Djouadi

Robert

d’Hendecourt

et al. 2011

A&A

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Context. Interstellar silicate grains are thought to be amorphized by interaction with high-and low-energy particle interactions in astrophysical environments. In addition, low energy (a few keV) particles will implant atoms within the grains. Aims. In this paper we experimentally investigate the consequence of the implantation of H + at low irradiation energies into analogues of interstellar silicate grains, and look for the formation of hydroxyl radicals within the silicate matrix. Methods. Thin amorphous silicate films (∼100 nm) were sequentially irradiated with H + ions at low energies (3.5, 2.5 and then 1.5 keV) ensuring an implantation of the ions through the full depth of the films. The fluences used, 3× 10 16 , 10 17 and 3× 10 17 H + /cm 2 , are compatible with those expected in shocks in the interstellar medium. We used infrared spectroscopy to monitor and quantify the OH band evolution after irradiation. In order to distinguish the newly formed OH groups from those originating from unavoidable atmospheric contamination, the D/H depth ratios were measured with a NanoSIMS ion microprobe.Results. An increase in the OH band strength in the infrared spectra after irradiation reveals the formation of OH bonds within the irradiated silicate thin films. NanoSIMS measurements of the D/H signature in the region of ion implantation show that the newlyformed OH groups make up about 40% of the observed OH band in the IR, the rest are due to an atmospheric hydroxylation of the sample. Only about 2% of the incident ions lead to OH bond formation and, at most, the irradiated silicates retain about 3% of the incident protons as OH groups within their structure. Conclusions. Our laboratory experimental simulations show a possible production and storage of hydroxyl radicals in amorphous laboratory silicates. In the astrophysical context, such OH radicals, strongly bonded to pre-accretion material, could constitute a non negligible reservoir of -OH, thus water. These experimental results allow us to revisit and reinstate the hypothesis of a possible "wet" accretion of the telluric planets early in the history of the formation of the Solar System.

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“…Complex organic compounds were also found in comets by the direct analysis of the dust from Comet Halley with mass spectrometer on spacecraft 17) . Ground-based chemical analyses of cometary dust particles returned by Stardust mission have revealed more details of organic chemistry of Comet 81P/Wild 2 18,[30][31][32][33][34] .…”

Section: Analysis Of Organic Compounds In Interplanetary Dust Particlmentioning

confidence: 99%

“…The contribution in exogenous delivery of organic carbon to the early Earth might have been more than those from meteorites and comets, because (i) they contains higher amounts of organic carbon (ca. 10%) than meteorites 34) , (ii) the flux of IDPs is more steady and higher (40 x 10 4 t per year) than those of comets and meteorites 35) , and (iii) IDPs could have been decelerated during atmospheric entry to deliver their organics intact while the organics in comets and meteorites could have been vaporized or decomposed upon their impacts. However, the IDPs have been captured by aircrafts or on the surface of Earth for the analyses.…”

Section: Analysis Of Organic Compounds In Interplanetary Dust Particlmentioning

confidence: 99%

Tanpopo: Astrobiology Exposure and Micrometeoroid Capture Experiments— Proposed Experiments at the Exposure Facility of ISS-JEM

Yamagishi

Yokobori

Hashimoto

et al. 2014

AEROSPACE TECHNOLOGY JAPAN

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Carbon abundance and silicate mineralogy of anhydrous interplanetary dust particles

Cited by 161 publications

References 26 publications

Dust in the Solar System: Properties and Origins

Dust in the Solar System: Properties and Origins

Hydroxyl radical production and storage in analogues of amorphous interstellar silicates: a possible “wet” accretion phase for inner telluric planets

Tanpopo: Astrobiology Exposure and Micrometeoroid Capture Experiments— Proposed Experiments at the Exposure Facility of ISS-JEM

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