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    Hints for Icy Pebble Migration Feeding an Oxygen-rich Chemistry in the Inner Planet-forming Region of Disks

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    Banzatti_2020_ApJ_903_124.pdf
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    Author
    Banzatti, Andrea
    Pascucci, Ilaria cc
    Bosman, Arthur D.
    Pinilla, Paola
    Salyk, Colette
    Herczeg, Gregory J.
    Pontoppidan, Klaus M.
    Vazquez, Ivan
    Watkins, Andrew
    Krijt, Sebastiaan
    Hendler, Nathan
    Long, Feng cc
    Show allShow less
    Affiliation
    Univ Arizona, Dept Planetary Sci
    Univ Arizona, Dept Astron
    Issue Date
    2020-11-10
    Keywords
    Circumstellar disks
    Protoplanetary disks
    Planetary system formation
    Molecular spectroscopy
    Molecular gas
    Millimeter astronomy
    Infrared astronomy
    Pre-main sequence stars
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Banzatti, A., Pascucci, I., Bosman, A. D., Pinilla, P., Salyk, C., Herczeg, G. J., ... & Long, F. (2020). Hints for icy pebble migration feeding an oxygen-rich chemistry in the inner planet-forming region of disks. The Astrophysical Journal, 903(2), 124.
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2020. 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
    We present a synergic study of protoplanetary disks to investigate links between inner-disk gas molecules and the large-scale migration of solid pebbles. The sample includes 63 disks where two types of measurements are available: (1) spatially resolved disk images revealing the radial distribution of disk pebbles (millimeter to centimeter dust grains), from millimeter observations with the Atacama Large Millimeter/Submillimeter Array or the Submillimeter Array, and (2) infrared molecular emission spectra as observed with Spitzer. The line flux ratios of H2O with HCN, C2H2, and CO2 all anticorrelate with the dust disk radius R-dust, expanding previous results found by Najita et al. for HCN/H2O and the dust disk mass. By normalization with the dependence on accretion luminosity common to all molecules, only the H2O luminosity maintains a detectable anticorrelation with disk radius, suggesting that the strongest underlying relation is between H2O and R-dust. If R-dust is set by large-scale pebble drift, and if molecular luminosities trace the elemental budgets of inner-disk warm gas, these results can be naturally explained with scenarios where the inner disk chemistry is fed by sublimation of oxygen-rich icy pebbles migrating inward from the outer disk. Anticorrelations are also detected between all molecular luminosities and the infrared index n(13-30), which is sensitive to the presence and size of an inner-disk dust cavity. Overall, these relations suggest a physical interconnection between dust and gas evolution, both locally and across disk scales. We discuss fundamental predictions to test this interpretation and study the interplay between pebble drift, inner disk depletion, and the chemistry of planet-forming material.
    ISSN
    0004-6256
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/abbc1a
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/abbc1a
    Scopus Count
    Collections
    UA Faculty Publications

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