The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines
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Author
Pascucci, Ilaria
Banzatti, Andrea
Gorti, Uma

Fang, Min

Pontoppidan, Klaus
Alexander, Richard
Ballabio, Giulia
Edwards, Suzan
Salyk, Colette
Sacco, Germano
Flaccomio, Ettore
Blake, Geoffrey A.

Carmona, Andres
Hall, Cassandra
Kamp, Inga

Käufl, Hans Ulrich
Meeus, Gwendolyn
Meyer, Michael
Pauly, Tyler
Steendam, Simon
Sterzik, Michael
Affiliation
Univ Arizona, Lunar & Planetary LabIssue Date
2020-11-04
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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 JOURNALRights
© 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
0004-637XEISSN
1538-4357Version
Final published versionSponsors
NSFae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/abba3c