Comparing Wild 2 particles to chondrites and IDPs

Zolensky, M. E.; Nakamura‐Messenger, K.; Rietmeijer, Frans J. M.; Leroux, Hugues; Mikouchi, T.; Ohsumi, Kazumasa; Simon, S. B.; Grossman, Lawrence; Stephan, T.; Weisberg, M. K.; Velbel, M. A.; Zega, T. J.; Stroud, Rhonda M.; Tomeoka, Kazushige; Ohnishi, Ichiro; Tomioka, Naotaka; Nakamura, Tomoki; Matrajt, G.; Joswiak, D. J.; Brownlee, D. E.; Langenhorst, F.; Krot, Alexander N.; Kearsley, A. T.; Ishii, H. A.; Graham, G. A.; Dai, Z. R.; Chi, Miaofang; Bradley, J. P.; Hagiya, Kenji; Gounelle, M.; Keller, L. P.; Bridges, J. C.

doi:10.1111/j.1945-5100.2008.tb00621.x

Cited by 149 publications

(153 citation statements)

References 45 publications

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“…Our spectral decomposition results suggest that the crystalline olivine grains in the inner belt contain more Fe than is expected for comet-like bodies (Wooden 2008;Zolensky et al 2008;Hanner & Zolensky 2010). Similar results were also found for cold crystalline olivine grains observed in other debris disks (β Pic, de Vries et al 2012), and protoplanetary disks (e.g., Olofsson et al 2010;Sturm et al 2010Sturm et al , 2013.…”

Section: The Origin Of Transient Dustsupporting

confidence: 75%

The twofold debris disk around HD 113766 A

Olofsson

Henning

Nielbock

et al. 2013

A&A

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Context. Warm debris disks are a sub-sample of the large population of debris disks, and display excess emission in the mid-infrared. Around solar-type stars, very few objects (∼2% of all debris disks) show emission features in mid-IR spectroscopic observations that are attributed to small, warm silicate dust grains. The origin of this warm dust could be explained either by a recent catastrophic collision between several bodies or by transport from an outer belt similar to the Kuiper belt in the solar system.Aims. We present and analyze new far-IR Herschel/PACS photometric observations, supplemented by new and archival ground-based data in the mid-IR (VLTI/MIDI and VLT/VISIR), for one of these rare systems: the 10-16 Myr old debris disk around HD 113766 A. We improve an existing model to account for these new observations. Methods. We implemented the contribution of an outer planetesimal belt in the D code, and successfully used it to model the spectral energy distribution (SED) as well as complementary observations, notably MIDI data. We better constrain the spatial distribution of the dust and its composition. Results. We underline the limitations of SED modeling and the need for spatially resolved observations. We improve existing models and increase our understanding of the disk around HD 113766 A. We find that the system is best described by an inner disk located within the first AU, well constrained by the MIDI data, and an outer disk located between 9-13 AU. In the inner dust belt, our previous finding of Fe-rich crystalline olivine grains still holds. We do not observe time variability of the emission features over at least an eight-year time span in an environment subjected to strong radiation pressure. Conclusions. The time stability of the emission features indicates that µm-sized dust grains are constantly replenished from the same reservoir, with a possible depletion of sub-µm-sized grains. We suggest that the emission features may arise from multi-composition aggregates. We discuss possible scenarios concerning the origin of the warm dust observed around HD 113766 A. The compactness of the innermost regions as probed by the MIDI visibilities and the dust composition suggest that we are witnessing the results of (at least) one collision between partially differentiated bodies, in an environment possibly rendered unstable by terrestrial planetary formation.

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Section: The Origin Of Transient Dustsupporting

confidence: 75%

The twofold debris disk around HD 113766 A

Olofsson

Henning

Nielbock

et al. 2013

A&A

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“…Microchondrule-like objects with textural, mineralogical and isotopic properties of chondrules in carbonaceous chondrites have also recently been found in Wild 2 samples . Their presence as well as that of a CAI in the Stardust samples has been attributed to a large scale mixing of high-temperature minerals formed in the inner solar system Nakamura et al, 2008;Simon et al, 2008).…”

Section: Anhydrous Idpsmentioning

confidence: 99%

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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“…For both comets, the mineralogical findings echo the results from the Stardust mission on comet P81/Wild 2. Based on samples collected in situ, Zolensky et al (2008) found that olivines in the comet mostly consist of Mg-rich olivine grains, with a Mg fraction (=Mg / [Mg + Fe]) of about 99. However, they also found the composition range of olivine to be extremely broad, ranging from Mg fractions between 4 and 100.…”

Section: Cometary Bodiesmentioning

confidence: 99%

Transient dust in warm debris disks

Olofsson

Juhász

Henning

et al. 2012

A&A

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Context. Debris disks trace remnant reservoirs of leftover planetesimals in planetary systems. In the past years, a handful of "warm" debris disks have been discovered in which emission in excess starts in the mid-infrared. An interesting subset of these warm debris disks shows emission features in mid-infrared spectra, which points towards the presence of μm-sized dust grains, with temperatures above hundreds K. Given the ages of the host stars, the presence of these small grains is puzzling, and raises questions about their origin and survival in time.Aims. This study focuses on determining the mineralogy of the dust around seven debris disks with evidence for warm dust, based on Spitzer/IRS spectroscopic data, to provide new insights into the origin of the dust grains. Methods. We developed and present a new radiative transfer code (Debra) dedicated to spectral energy distribution (SED) modeling of optically thin disks. The Debra code is designed such that it can simultaneously determine dust composition and disk properties. We used this code on the SEDs of seven warm debris disks, in combination with recent laboratory experiments on dust optical properties. Results. We find that most, if not all, debris disks in our sample are experiencing a transient phase, suggesting a production of small dust grains on relatively short timescales. Dust replenishment should be efficient on timescales of months for at least three sources. From a mineralogical point of view, we find that crystalline pyroxene grains (enstatite) have low abundances compared to crystalline olivine grains. The main result of our study is that we find evidence for Fe-rich crystalline olivine grains (Fe/[Mg + Fe] ∼ 0.2) for several debris disks. This finding contrasts with studies of gas-rich protoplanetary disks, where Fe-bearing crystalline grains are usually not observed. Conclusions. These Fe-rich olivine grains, and the overall differences between the mineralogy of dust in Class II disks compared to debris disks suggests that the transient crystalline dust in warm debris disk is of a new generation. We discuss possible crystallization routes to explain our results, and also comment on the mechanisms that may be responsible for the production of small dust grains.

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Comparing Wild 2 particles to chondrites and IDPs

Abstract: Comparing Wild 2 particles to chondrites and IDPs

Cited by 149 publications

References 45 publications

The twofold debris disk around HD 113766 A

The twofold debris disk around HD 113766 A

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

Transient dust in warm debris disks

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