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

Pascucci, Ilaria and Banzatti, Andrea and Gorti, Uma and Fang, Min and Pontoppidan, Klaus and Alexander, Richard and Ballabio, Giulia and Edwards, Suzan and Salyk, Colette and Sacco, Germano and Flaccomio, Ettore and Blake, Geoffrey A. and Carmona, Andres and Hall, Cassandra and Kamp, Inga and Käufl, Hans Ulrich and Meeus, Gwendolyn and Meyer, Michael and Pauly, Tyler and Steendam, Simon and Sterzik, Michael (2020) The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines. Astrophysical Journal, 903 (2). Art. No. 78. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20201104-152958678

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Abstract

We analyze high-resolution (Δv ≤ 10 km s⁻¹) optical and infrared spectra covering the [O I] λ6300 and [Ne II] 12.81 μm 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_(acc) > 10⁻⁸M_⊙ yr⁻¹), while LVCs are found in sources with low M_(acc), low [O I] luminosity, and large infrared spectral index (n₁₃₋₃₁). Interestingly, the [Ne II] and [O I] LVC luminosities display an opposite behavior with n₁₃₋₃₁: as the inner dust disk depletes (higher n₁₃₋₃₁), 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 (~1 keV) X-rays in inner, mostly molecular, MHD winds.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/abba3cDOIArticle
https://arxiv.org/abs/2009.09114arXivDiscussion Paper
ORCID:
AuthorORCID
Pascucci, Ilaria0000-0001-7962-1683
Banzatti, Andrea0000-0003-4335-0900
Gorti, Uma0000-0002-3311-5918
Fang, Min0000-0001-8060-1321
Pontoppidan, Klaus0000-0001-7552-1562
Alexander, Richard0000-0001-6410-2899
Edwards, Suzan0000-0002-3232-665X
Salyk, Colette0000-0003-3682-6632
Sacco, Germano0000-0002-6893-2221
Flaccomio, Ettore0000-0002-3638-5788
Blake, Geoffrey A.0000-0003-0787-1610
Carmona, Andres0000-0003-2471-1299
Hall, Cassandra0000-0002-8138-0425
Kamp, Inga0000-0001-7455-5349
Käufl, Hans Ulrich0000-0002-8806-9795
Meeus, Gwendolyn0000-0002-6251-0108
Meyer, Michael0000-0003-1227-3084
Pauly, Tyler0000-0001-9500-9267
Sterzik, Michael0000-0002-5784-4437
Additional Information:© 2020 The American Astronomical Society. Received 2020 June 9; revised 2020 August 26; accepted 2020 September 16; published 2020 November 4. This work is based on observations collected at the European Southern Observatory under ESO program 198.C-0104. I.P., U.G., and S.E. acknowledge support from a Collaborative NSF Astronomy & Astrophysics Research grant (ID: 1715022, ID:1713780, and ID:1714229). This material is based on work supported by the National Aeronautics and Space Administration under agreement No. NNX15AD94G for the program Earths in Other Solar Systems. The results reported herein benefited from collaborations and/or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. R.D.A., G.B., and C.H. acknowledge funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 681601). G.B. acknowledges support from the University of Leicester through a College of Science and Engineering PhD studentship. C.H. is a Winton Fellow, and this research has been supported by Winton Philanthropies/The David and Claudia Harding Foundation. This project has been carried out as part of the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 823823 (dustbusters). Facility: ESO(VISIR). - Software: astropy (The Astropy Collaboration et al. 2013, 2018), mpfitfun (MINPACK-1 in Jorge Moré & Stephen Wright 1987), cenken (Helsel 2005 and Akritas et al. 1995).
Funders:
Funding AgencyGrant Number
NSFAST-1715022
NSFAST-1713780
NSFAST-1714229
NASANNX15AD94G
European Research Council (ERC)681601
University of LeicesterUNSPECIFIED
Winton PhilanthropiesUNSPECIFIED
David and Claudia Harding FoundationUNSPECIFIED
Marie Curie Fellowship823823
Subject Keywords:Protoplanetary disks ; Stellar accretion disks ; Stellar jets
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Protoplanetary disks (1300); Stellar accretion disks (1579); Stellar jets (1607)
Record Number:CaltechAUTHORS:20201104-152958678
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20201104-152958678
Official Citation:Ilaria Pascucci et al 2020 ApJ 903 78
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:106440
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:05 Nov 2020 00:19
Last Modified:05 Nov 2020 00:19

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