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

Andrea Banzatti, Ilaria Pascucci, Suzan Edwards, Min Fang, Uma Gorti, Mario Flock

Research output: Contribution to journalArticle

5 Citations (Scopus)

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 ("BC" and "NC," 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 ("SCJ") and those that do not ("SC"). 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.

Original languageEnglish (US)
Article number76
JournalAstrophysical Journal
Volume870
Issue number2
DOIs
StatePublished - Jan 10 2019

Fingerprint

coevolution
kinematics
high resolution
low speed
accretion
tracing
light emission
dust
luminosity
radii
T Tauri stars
wind velocity
high temperature gases
spectral resolution
centroids
depletion

Keywords

  • circumstellar matter
  • ISM: jets and outflows
  • protoplanetary disks
  • stars: pre-main sequence
  • stars: winds, outflows

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Kinematic Links and the Coevolution of MHD Winds, Jets, and Inner Disks from a High-resolution Optical [O I] Survey. / Banzatti, Andrea; Pascucci, Ilaria; Edwards, Suzan; Fang, Min; Gorti, Uma; Flock, Mario.

In: Astrophysical Journal, Vol. 870, No. 2, 76, 10.01.2019.

Research output: Contribution to journalArticle

Banzatti, Andrea ; Pascucci, Ilaria ; Edwards, Suzan ; Fang, Min ; Gorti, Uma ; Flock, Mario. / Kinematic Links and the Coevolution of MHD Winds, Jets, and Inner Disks from a High-resolution Optical [O I] Survey. In: Astrophysical Journal. 2019 ; Vol. 870, No. 2.
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AB - 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 ("BC" and "NC," 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 ("SCJ") and those that do not ("SC"). 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.

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