The retention of dust in protoplanetary disks: evidence from agglomeration olivine chondrules from the outer solar system

S.R. Waitukaitis, D. Schrader, K. Nagashima, J. Davidson, T. Mccoy, H. Conolly Jr, D. Lauretta, Geochimica et Cosmochimica Acta 223 (2018) 405–421.

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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.
Publishing Year
Date Published
2018-02-15
Journal Title
Geochimica et Cosmochimica Acta
Volume
223
Page
405 - 421
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Waitukaitis SR, Schrader D, Nagashima K, et al. The retention of dust in protoplanetary disks: evidence from agglomeration olivine chondrules from the outer solar system. Geochimica et Cosmochimica Acta. 2018;223:405-421. doi:10.1016/j.gca.2017.12.014
Waitukaitis, S. R., Schrader, D., Nagashima, K., Davidson, J., Mccoy, T., Conolly Jr, H., & Lauretta, D. (2018). The retention of dust in protoplanetary disks: evidence from agglomeration olivine chondrules from the outer solar system. Geochimica et Cosmochimica Acta, 223, 405–421. https://doi.org/10.1016/j.gca.2017.12.014
Waitukaitis, Scott R, Devin Schrader, Kazuhide Nagashima, Jemma Davidson, Timothy Mccoy, Harold Conolly Jr, and Dante Lauretta. “The Retention of Dust in Protoplanetary Disks: Evidence from Agglomeration Olivine Chondrules from the Outer Solar System.” Geochimica et Cosmochimica Acta 223 (2018): 405–21. https://doi.org/10.1016/j.gca.2017.12.014.
S. R. Waitukaitis et al., “The retention of dust in protoplanetary disks: evidence from agglomeration olivine chondrules from the outer solar system,” Geochimica et Cosmochimica Acta, vol. 223, pp. 405–421, 2018.
Waitukaitis SR, Schrader D, Nagashima K, Davidson J, Mccoy T, Conolly Jr H, Lauretta D. 2018. The retention of dust in protoplanetary disks: evidence from agglomeration olivine chondrules from the outer solar system. Geochimica et Cosmochimica Acta. 223, 405–421.
Waitukaitis, Scott R., et al. “The Retention of Dust in Protoplanetary Disks: Evidence from Agglomeration Olivine Chondrules from the Outer Solar System.” Geochimica et Cosmochimica Acta, vol. 223, Elsevier, 2018, pp. 405–21, doi:10.1016/j.gca.2017.12.014.

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