Locating the Launching Region of T Tauri Winds: The Case of DG Tauri
By Jeffrey M. Anderson, Zhi-Yun Li, Ruben Krasnopolsky, R. Blandford. 2003
155 citations recorded by the source corpus.
It is widely believed that T Tauri winds are driven magnetocentrifugally from accretion disks close to the central stars. The exact launching conditions are uncertain. We show that a general relation exists between the poloidal and toroidal velocity components of a magnetocentrifugal wind at large distances and the rotation rate of the launching surface, independent of the uncertain launching conditions. We discuss the physical basis of this relation and verify it by using a set of numerically determined large-scale wind solutions. Both velocity components are in principle measurable from spatially resolved spectra, as has been done for the extended low-velocity component (LVC) of the DG Tauri wind by Bacciotti et al. For this particular source, we infer that the spatially resolved LVC originates from a region on the disk extending from ~0.3 to ~4.0 AU from the star, which is consistent with, and a refinement over, the rough estimate of Bacciotti et al.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/edeadf83a618c062ef95a712a6672aed5263cb73
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In Astronomy and Astrophysics
Citations in the corpus
- Accretion-powered Stellar Winds as a Solution to the Stellar Angular Momentum Problem (2005, unknown): “Thus, CTTS winds should rotate at a speed comparable to that of a disk wind (Bacciotti et al. 2002; Anderson et al. 2003) at observationally resolved distances from the star.”
- Which jet launching mechanism(s) in T Tauri stars (2006, methodology): “Anderson et al. (2003) further demonstrated that the launching radius of a keplerian disc wind may be simply derived from the jet rotation and poloidal speeds once the stellar mass is known, regardless of the details of the MHD disc wind solution.”
- Rotation of Jets from Young Stars: New Clues from the Hubble Space Telescope Imaging Spectrograph (2003, methodology): “Using Equation 1 (Anderson et al. 2003), ̟0 ≈ 0.7AU ( ̟∞ 10AU )2/3 ( vφ,∞ 10kms−1 )2/3 × ( vp,∞ 100kms−1 )−4/3 ( M⋆ 1M⊙ )1/3 (1) and assuming all three sources are of mass M⋆ ∼ 1M⊙, which is a reasonable approximation given the weak dependence on M⋆, we obtain values for ̟0 as shown in Table 4.”
- Kinematics of the jet in M 87 on scales of 100–1000 Schwarzschild radii (2016, background): “…of jet rotation has been previously reported in jets from young stellar objects (YSO), based on spectroscopic radial velocity analysis (e.g. Anderson et al. 2003; Choi et al. 2011), and has been successfully associated with an MHD process, giving a constraint on the jet launching location.”
- Accretion-powered Stellar Winds. II. Numerical Solutions for Stellar Wind Torques (2008, background): “…momenta of the outflows (Königl & Pudritz 2000), the X-ray luminosities (Decampli 1981), and possible detection of rotation (Bacciotti et al. 2002; Anderson et al. 2003; Coffey et al. 2004; Ferreira et al. 2006; Coffey et al. 2007), it appears that most of the flow arises from the accretion…”
- Photoevaporation of Circumstellar Disks around Young Stars (2004, background): “In fact, the prevailing view is that T Tauri winds are magnetically-driven (e.g., Anderson et al. 2003).”
- Theory of Star Formation (2007, background): “For the low velocity component of DG Tau, Anderson et al. (2003) find from calculating Ω0 as above that the wind launch point radii are ∼ 0.3−4AU, implying a disk wind.”