English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

Kinematic Links and the Coevolution of MHD Winds, Jets, and Inner Disks from a High-resolution Optical [O I] Survey

MPS-Authors

Banzatti,  Andrea
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pascucci,  Ilaria
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Edwards,  Suzan
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fang,  Min
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gorti,  Uma
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Flock,  Mario
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Ressource
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Banzatti, A., Pascucci, I., Edwards, S., Fang, M., Gorti, U., & Flock, M. (2019). Kinematic Links and the Coevolution of MHD Winds, Jets, and Inner Disks from a High-resolution Optical [O I] Survey. The Astrophysical Journal, 870.


Cite as: http://hdl.handle.net/21.11116/0000-0005-D42F-8
Abstract
We present a survey of optical [O I] emission at 6300 Å toward 65 T Tauri stars at the spectral resolution of ~7 km s-1. Past work identified a highly blueshifted velocity component (HVC) tracing microjets and a less blueshifted low-velocity component (LVC) attributed to winds. We focus here on the LVC kinematics to investigate links between winds, jets, accretion, and disk dispersal. We track the behavior of four types of LVC components: a broad and a narrow component (‚ÄúBC‚Äù and ‚ÄúNC,‚Äù respectively) in LVCs that are decomposed into two Gaussians which typically have an HVC, and single-Gaussian LVC profiles separated into those that have an HVC (‚ÄúSCJ‚Äù) and those that do not (‚ÄúSC‚Äù). The LVC centroid velocities and line widths correlate with the HVC EW and accretion luminosity, suggesting that LVC/winds and HVC/jets are kinematically linked and connected to accretion. The deprojected HVC velocity correlates with accretion luminosity, showing that faster jets come with higher accretion. BC and NC kinematics correlate, and their blueshifts are maximum at ~35¬∞, suggesting a conical wind geometry with this semi-opening angle. Only SCs include n 13-31 up to ~3, and their properties correlate with this infrared index, showing that [O I] emission recedes to larger radii as the inner dust is depleted, tracing less dense/hot gas and a decrease in wind velocity. Altogether, these findings support a scenario where optically thick, accreting inner disks launch radially extended MHD disk winds that feed jets, and where inner disk winds recede to larger radii and jets disappear in concert with dust depletion.