The retention of dust in protoplanetary disks: Evidence from agglomeratic olivine chondrules from the outer Solar System

Devin Schrader, Kazuhide Nagashima, Scott R. Waitukaitis, Jemma Davidson, Timothy J. McCoy, Harold C. Connolly, Dante S. Lauretta

Research output: Contribution to journalArticle

7 Citations (Scopus)

Abstract

By investigating the in situ chemical and O-isotope compositions of olivine in lightly sintered dust agglomerates from the early Solar System, we constrain their origins and the retention of dust in the protoplanetary disk. The grain sizes of silicates in these agglomeratic olivine (AO) chondrules indicate that the grain sizes of chondrule precursors in the Renazzo-like carbonaceous (CR) chondrites ranged from <1 to 80 µm. We infer this grain size range to be equivalent to the size range for dust in the early Solar System. AO chondrules may contain, but are not solely composed of, recycled fragments of earlier formed chondrules. They also contain 16O-rich olivine related to amoeboid olivine aggregates and represent the best record of chondrule-precursor materials. AO chondrules contain one or more large grains, sometimes similar to FeO-poor (type I) and/or FeO-rich (type II) chondrules, while others contain a type II chondrule core. These morphologies are consistent with particle agglomeration by electrostatic charging of grains during collision, a process that may explain solid agglomeration in the protoplanetary disk in the micrometer size regime. The petrographic, isotopic, and chemical compositions of AO chondrules are consistent with chondrule formation by large-scale shocks, bow shocks, and current sheets. The petrographic, isotopic, and chemical similarities between AO chondrules in CR chondrites and chondrule-like objects from comet 81P/Wild 2 indicate that comets contain AO chondrules. We infer that these AO chondrules likely formed in the inner Solar System and migrated to the comet forming region at least 3 Ma after the formation of the first Solar System solids. Observations made in this study imply that the protoplanetary disk retained a dusty disk at least ∼3.7 Ma after the formation of the first Solar System solids, longer than half of the dusty accretion disks observed around other stars.

Original languageEnglish (US)
Pages (from-to)405-421
Number of pages17
JournalGeochimica et Cosmochimica Acta
Volume223
DOIs
StatePublished - Feb 15 2018

Fingerprint

chondrule
Solar system
solar system
Dust
olivine
dust
comet
grain size
carbonaceous chondrite
Agglomeration
agglomeration
Silicates
Chemical analysis
Isotopes
Stars
Electrostatics
range size

Keywords

  • Agglomeratic olivine chondrule
  • Asteroid
  • Comet Wild 2
  • CR chondrite
  • Oxygen isotopes
  • Protoplanetary disk

ASJC Scopus subject areas

  • Geochemistry and Petrology

Cite this

The retention of dust in protoplanetary disks : Evidence from agglomeratic olivine chondrules from the outer Solar System. / Schrader, Devin; Nagashima, Kazuhide; Waitukaitis, Scott R.; Davidson, Jemma; McCoy, Timothy J.; Connolly, Harold C.; Lauretta, Dante S.

In: Geochimica et Cosmochimica Acta, Vol. 223, 15.02.2018, p. 405-421.

Research output: Contribution to journalArticle

Schrader, Devin ; Nagashima, Kazuhide ; Waitukaitis, Scott R. ; Davidson, Jemma ; McCoy, Timothy J. ; Connolly, Harold C. ; Lauretta, Dante S. / The retention of dust in protoplanetary disks : Evidence from agglomeratic olivine chondrules from the outer Solar System. In: Geochimica et Cosmochimica Acta. 2018 ; Vol. 223. pp. 405-421.
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