Tracing Slow Winds From T Tauri Stars via Low-Velocity Forbidden Line Emission

Molly N. Simon, University of Arizona
Ilaria Pascucci, University of Arizona
Suzan Edwards, Smith College
W. Feng, Arizona State University at the Tempe Campus
Uma Gorti, SETI Institute
D. Hollenbach, SETI Institute
E. Rigliaco, Institute for Astronomy
James T. Keane, University of Arizona

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Using Keck/HIRES spectra (Δ v∼7 km s−1) we analyze forbidden lines of [O I] 6300 Å, [OI] 5577 Å and [SII]6731 Å from 33 T Tauri stars covering a range of disk evolutionary stages. After removing a high-velocity component (HVC) associated with microjets, we study the properties of the low-velocity component (LVC). The LVC can be attributed to slow disk winds that could be magnetically (magnetohydrodynamic) or thermally(photoevaporative) driven. Both of these winds play an important role in the evolution and dispersal of protoplanetary material. LVC emission is seen in all 30 stars with detected [OI] but only in two out of eight with detected [SII], so our analysis is largely based on the properties of the [OI] LVC. The LVC itself is resolved into broad (BC) and narrow (NC) kinematic components. Both components are found over a wide range of accretion rates and their luminosity is correlated with the accretion luminosity, but the NC is proportionately stronger than the BC in transition disks. The full width at half maximum of both the BC and NC correlates with disk inclination, consistent with Keplerian broadening from radii of 0.05 to 0.5 au and 0.5 to 5 au, respectively. The velocity centroids of the BC suggest formation in an MHD disk wind, with the largest blueshifts found in sources with closer to face-on orientations. The velocity centroids of the NC, however, show no dependence on disk inclination. The origin of this component is less clear and the evidence for photoevaporation is not conclusive.