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    The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines

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    Pascucci_2020_ApJ_903_78.pdf
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    Author
    Pascucci, Ilaria cc
    Banzatti, Andrea
    Gorti, Uma cc
    Fang, Min cc
    Pontoppidan, Klaus
    Alexander, Richard
    Ballabio, Giulia
    Edwards, Suzan
    Salyk, Colette
    Sacco, Germano
    Flaccomio, Ettore
    Blake, Geoffrey A. cc
    Carmona, Andres
    Hall, Cassandra
    Kamp, Inga cc
    Käufl, Hans Ulrich
    Meeus, Gwendolyn
    Meyer, Michael
    Pauly, Tyler
    Steendam, Simon
    Sterzik, Michael
    Show allShow less
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2020-11-04
    Keywords
    Protoplanetary disks
    Stellar acccretion disks
    Stellar jets
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Pascucci, I., Banzatti, A., Gorti, U., Fang, M., Pontoppidan, K., Alexander, R., ... & Sterzik, M. (2020). The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines. The Astrophysical Journal, 903(2), 78.
    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 analyze high-resolution (Delta v <= 10 km s(-1)) optical and infrared spectra covering the [O i] lambda 6300 and [Ne II] 12.81 mu m lines from a sample of 31 disks in different evolutionary stages. Following work at optical wavelengths, we use Gaussian profiles to fit the [Ne II] lines and classify them into high-velocity component (HVC) or low-velocity component (LVC) if the line centroid is more or less blueshifted than 30 km s(-1) with respect to the stellar radial velocity, respectively. Unlike for the [O I], where an HVC Is often accompanied by an LVC, all 17 sources with an [Ne II] detection have either an HVC or an LVC. [Ne II] HVCs are preferentially detected toward high accretors ((M) over dot(ace) > 10(-8) M-circle dot yr(-1)), while LVCs are found In sources with low M-acc, low [O I] luminosity, and large Infrared spectral Index (n(13-31)). Interestingly, the [Ne II] and [O I] LVC luminosities display an opposite behavior with n(13-31): as the Inner dust disk depletes (higher n(13-31)), the [Ne II] luminosity Increases while the [O I] weakens. The [Ne II] and [O I] HVC profiles are generally similar, with centroids and FWHMs showing the expected behavior from shocked gas In microjets. In contrast, the [Ne II] LVC profiles are typically more blueshifted and narrower than the [O I] profiles. The FWHM and centroid versus disk Inclination suggest that the [Ne II] LVC predominantly traces unbound gas from a slow, wide-angle wind that has not lost completely the Keplerian signature from Its launching region. We sketch an evolutionary scenario that could explain the combined [O I] and [Ne II] results and Includes screening of hard (similar to 1 keV) X-rays In Inner, mostly molecular, MHD winds.
    ISSN
    0004-637X
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/abba3c
    Version
    Final published version
    Sponsors
    NSF
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/abba3c
    Scopus Count
    Collections
    UA Faculty Publications

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