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    Dust Transport and Processing in Centrifugally Driven Protoplanetary Disk Winds

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    Giacalone_2019_ApJ_882_33.pdf
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    1.311Mb
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    PDF
    Description:
    Final Published Version
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    Author
    Giacalone, Steven
    Teitler, Seth
    Königl, Arieh
    Krijt, Sebastiaan
    Ciesla, Fred J.
    Affiliation
    Univ Arizona, Dept Astron & Steward Observ
    Issue Date
    2019-08-29
    Keywords
    circumstellar matter
    ISM: jets and outflows
    ISM: magnetic fields
    protoplanetary disks
    stars: protostars
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Steven Giacalone et al 2019 ApJ 882 33
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    Copyright © 2019. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    There is evidence that protoplanetary disks including the protosolar one-contain crystalline dust grains on spatial scales where the dust temperature is lower than the threshold value for their formation through thermal annealing of amorphous interstellar silicates. We interpret these observations in terms of an extended, magnetocentrifugally driven disk wind that transports grains from the inner disk-where they are thermally processed by the stellar radiation after being uplifted from the disk surfaces-to the outer disk regions. For any disk radius r, there is a maximum grain size a(max)(r) that can be uplifted from that location: grains of size a << a(max) are carried away by the wind, whereas those with a less than or similar to a(max) reenter the disk at larger radii. A significant portion of the reentering grains converge to-and subsequently accumulate in-a narrow region just beyond r(max)(a), the maximum radius from which grains of size a can be uplifted. We show that this model can account for the inferred crystallinity fractions in classical T Tauri and Herbig Ae disks and for their indicated near constancy after being established early in the disk evolution. It is also consistent with the reported radial gradients in the mean grain size, crystallinity, and crystal composition. In addition, this model yields the properties of the grains that remain embedded in the outflows from protoplanetary disks and naturally explains the inferred persistence of small grains in the surface layers of these disks.
    ISSN
    0004-637X
    DOI
    10.3847/1538-4357/ab311a
    Version
    Final published version
    Sponsors
    NASA ATP grant [NNX13AH56G]; Hubble Fellowship Program by NASA through Space Telescope Science Institute [HST-HF2-51394.002-A]; NASANational Aeronautics & Space Administration (NASA) [NAS 5-26555]
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab311a
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