^1,2Kainen L.Utt,^1,2Ryan C.Ogliore,^1,2Nan Liu,³Alexander N.Krot,³John P.Bradley,⁴Donald E.Brownlee,⁴David J.Joswiak
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2022.11.020]
¹Department of Physics, Washington University in St. Louis, St. Louis, MO 63130
²McDonnell Center for the Space Sciences, Washington University in St. Louis, St. Louis, MO 63130
³Hawaii Institute of Geophysics and Planetology, University of Hawaii at Mānoa, Honolulu, HI 96822
⁴Department of Astronomy, University of Washington, Seattle, WA 98195
Copyright Elsevier

Filamentary enstatite crystals, formed by gas-solid condensation in the solar nebula, are found in chondritic porous interplanetary dust particles of probable cometary origin. We measured the oxygen isotopic composition of four filamentary enstatite grains, two whiskers (1.8μm and 2.3μm in length) and two ribbons (3.4μm and 6.1μm in length), from the giant cluster interplanetary dust particle U2-20 GCP using NanoSIMS ion imaging. These grains represent both the ¹⁶O-rich solar (δ^17,18O ≈-70 ‰) and ¹⁶O-poor planetary (δ^17,18O ≈0 ‰) isotope reservoirs. Our measurements provide evidence for very early vaporization of dust-poor and dust-rich regions of the solar nebula, followed by condensation and outward transport of crystalline dust to the comet-forming region very far from the Sun. Similar processes are likely responsible for the crystalline silicates observed in the outer regions of protoplanetary disks elsewhere in the Galaxy.