An asteroidal breccia: The anatomy of a cluster IDP

Thomas, K. L.; Blanford, G. E.; Clemett, S. J.; Flynn, G. J.; Keller, L. P.; Klöck, W.; Maechling, C. R.; Kay, D.S. Mc; Messenger, S.; Nier, Alfred O.; Schlutter, D. J.; Sutton, S. R.; Warren, Jack L.; Zare, Richard N.

doi:10.1016/0016-7037(95)00174-x

Cited by 61 publications

(40 citation statements)

References 34 publications

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“…Jedwab, 1971) and is different from that of magnetite rims formed during atmospheric entry heating, either as nanocrystals (IDPs, e.g. Fraundorf, 1981;Thomas et al, 1995), skeletal crystals (AMMs, Toppani et al, 2001)o r euhedral crystals embedded in silicate glass (AMMs, Toppani et al, 2001). In addition, similar magnetite framboids were previously reported in hydrated IDPs attributed to a CI parent body (e.g.…”

Section: Hydrated Idpsmentioning

confidence: 72%

Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets

Adnot

Engrand

Leshin

et al. 2009

Geochimica et Cosmochimica Acta

108

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. Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets. Geochimica et Cosmochimica Acta, Elsevier, 2009, 73, pp.4558-4575. 10 Abstract Oxygen isotopes were measured in four chondritic hydrated interplanetary dust particles (IDPs) and five chondritic anhydrous IDPs including two GEMS-rich particles (Glass embedded with metal and sulfides) by a combination of high precision and high lateral resolution ion microprobe techniques.All IDPs have isotopic compositions tightly clustered around that of solar system planetary materials. Hydrated IDPs have mass-fractionated oxygen isotopic compositions similar to those of CI and CM carbonaceous chondrites, consistent with hydration of initially anhydrous protosolar dust. Anhydrous IDPs have small 16 O excesses and depletions similar to those of carbonaceous chondrites, the largest 16 O variations being hosted by the two GEMS-rich IDPs. Coarse-grained forsteritic olivine and enstatite in anhydrous IDPs are isotopically similar to their counterparts in comet Wild 2 and in chondrules suggesting a high temperature inner solar system origin. The small variations in the 16 O content of GEMS-rich IDPs suggest that most GEMS either do not preserve a record of interstellar processes or the initial interstellar dust is not 16 O-rich as expected by self-shielding models, although a larger dataset is required to verify these conclusions.Together with other chemical and mineralogical indicators, O isotopes show that the parent-bodies of carbonaceous chondrites, of chondritic IDPs, of most Antarctic micrometeorites, and comet Wild 2 belong to a single family of objects of carbonaceous chondrite chemical affinity as distinct from ordinary, enstatite, K-and R-chondrites. Comparison with astronomical observations thus suggests a chemical continuum of objects including main belt and outer solar system asteroids such as C-type, P-type and D-type asteroids, Trojans and Centaurs as well as short-period comets and other Kuiper Belt Objects.

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Section: Hydrated Idpsmentioning

confidence: 72%

Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets

Adnot

Engrand

Leshin

et al. 2009

Geochimica et Cosmochimica Acta

108

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“…This behavior is consistent with fluffy particle fragmentation (Fulle et al 2015a). Morphological analogs could be explored among collected extraterrestrial dust particles: 1) the chondritic porous aggregates, the ultrafine-grained matrix with occasional micron-sized iron-sulfide and/or Mg-rich olivine grains (Rietmeijer 2002); 2) cluster IDPs, a mixture of micron-sized grains and 5−20 micron sulfide and silicate minerals (Rietmeijer & Nuth 2004;Thomas et al 1995); and 3) giant cluster IDPs (Messenger et al 2015). GIADA fluffy lowdensity aggregates analogs among the Wild 2 particles could be the volatile-rich aggregates producing bulbous tracks (type C, Hörz et al 2006), in the capturing aerogel, leaving organic IR features along the track and carbon-rich small fragments completely scattered throughout the track (Sandford et al 2006;Rotundi et al 2008).…”

Section: Discussionmentioning

confidence: 99%

GIADA: shining a light on the monitoring of the comet dust production from the nucleus of 67P/Churyumov-Gerasimenko

Corte

Rotundi

Fulle

et al. 2015

A&A

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oro.open.ac.uk Aims. We aim to describe the dust spatial distribution in the coma of comet 67P by means of in situ measurements. We determine dynamical and physical properties of cometary dust particles to support the study of the production process and dust environment modification. Methods. We analyzed GIADA data with respect to the observation geometry and heliocentric distance to describe the coma dust spatial distribution of 67P, to monitor its activity, and to retrieve information on active areas present on its nucleus. We combined GIADA detection information with calibration activity to distinguish different types of particles that populate the coma of 67P: compact particles and fluffy porous aggregates. By means of particle dynamical parameters measured by GIADA, we studied the dust acceleration region.Results. GIADA was able to distinguish different types of particles populating the coma of 67P: compact particles and fluffy porous aggregates. Most of the compact particle detections occurred at latitudes and longitudes where the spacecraft was in view of the comet's neck region of the nucleus, the so-called Hapi region. This resulted in an oscillation of the compact particle abundance with respect to the spacecraft position and a global increase as the comet moved from 3.36 to 2.43 AU heliocentric distance. The speed of these particles, having masses from 10 −10 to 10 −7 kg, ranged from 0.3 to 12.2 m s −1 . The variation of particle mass and speed distribution with respect to the distance from the nucleus gave indications of the dust acceleration region. The influence of solar radiation pressure on micron and submicron particles was studied. The integrated dust mass flux collected from the Sun direction, that is, particles reflected by solar radiation pressure, was three times higher than the flux coming directly from the comet nucleus. The awakening 67P comet shows a strong dust flux anisotropy, confirming what was suggested by on-ground dust coma observations performed in 2008.

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“…One of these contains the new mineral Brownleeite (Nakamura- Messenger et al 2010). However, given the chemical and mineralogic heterogeneity observed in different fragments from a single cluster IDP (Thomas et al 1995), the extent to which these compositional data are specifically applicable to the Suite 1 and 2 particles is uncertain.…”

Section: Sample Compositionsmentioning

confidence: 99%

Presolar Grains From Novae: Evidence From Neon and Helium Isotopes in Comet Dust Collections

Pepin

Palma

Gehrz

et al. 2011

ApJ

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Presolar grains in meteorites and interplanetary dust particles carry non-solar isotopic signatures pointing to origins in supernovae, giant stars, and possibly other stellar sources. There have been suggestions that some of these grains condensed in the ejecta of classical nova outbursts, but the evidence is ambiguous. We report neon and helium compositions in particles captured on stratospheric collectors flown to sample materials from comets 26P/Grigg-Skjellerup and 55P/Tempel-Tuttle that point to condensation of their gas carriers in the ejecta of a neon (ONe) nova. The absence of detectable 3 He in these particles indicates space exposure to solar wind irradiation of a few decades at most, consistent with origins in cometary dust streams. Measured

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An asteroidal breccia: The anatomy of a cluster IDP

Cited by 61 publications

References 34 publications

Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets

Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets

GIADA: shining a light on the monitoring of the comet dust production from the nucleus of 67P/Churyumov-Gerasimenko

Presolar Grains From Novae: Evidence From Neon and Helium Isotopes in Comet Dust Collections

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