2009.09114.pdf (1.55 MB)
Download file

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

Download (1.55 MB)
journal contribution
posted on 14.06.2021, 10:04 by Ilaria Pascucci, Andrea Banzatti, Uma Gorti, Min Fang, Klaus Pontoppidan, Richard Alexander, Giulia Ballabio, Suzan Edwards, Colette Salyk, Germano Sacco, Ettore Flaccomio, Geoffrey A Blake, Andres Carmona, Cassandra Hall, Inga Kamp, Hans Ulrich Kaeufl, Gwendolyn Meeus, Michael Meyer, Tyler Pauly, Simon Steendam, Michael Sterzik
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 lowvelocity 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 (Ṁacc > 10-8 Me⊙ yr-1), while LVCs are found in sources with low Ṁacc, 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.



2020 ApJ 903 78

Author affiliation

School of Physics and Astronomy


AM (Accepted Manuscript)

Published in

Astrophysical Journal






IOP Publishing for American Astronomical Society





Acceptance date


Copyright date


Available date