Rotation of Jets from Young Stars: New Clues from the Hubble Space Telescope Imaging Spectrograph
By D. Coffey, F. Bacciotti, J. Woitas, T. Ray, J. Eislöffel. 2003
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We report findings from the first set of data in a current survey to establish conclusively whether jets from young stars rotate. We observed the bipolar jets from the T Tauri stars TH 28 and RW Aur and the blueshifted jet from T Tauri star LkHα 321, using the Hubble Space Telescope Imaging Spectrograph. Forbidden emission lines show distinct and systematic velocity asymmetries of 10-25 (±5) km s-1 at a distance of 0.″3 from the source, representing a (projected) distance of ≈40 AU along the jet in the case of RW Aur, ≈50 AU for TH 28, and 165 AU in the case of LkHα 321. These velocity asymmetries are interpreted as rotation in the initial portion of the jet where it is accelerated and collimated. For the bipolar jets, both lobes appear to rotate in the same direction. Values obtained were in agreement with the predictions of MHD disk-wind models. Finally, we determine, from derived toroidal and poloidal velocities, values for the distance from the central axis of the footpoint for the jet's low-velocity component of ≈0.5-2 AU, consistent with the models of magnetocentrifugal launching.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/75e99bdc5a22c76797f91ebb8d045d1c7b13355a
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In Astronomy and Astrophysics
Citations in the corpus
- Magnetic tower outflows from a radial wire array Z-pinch (2005, background): “Recent observations of rotation in jets on ~ AU scales have provided new evidence for these models (Bacciotti et al. 2002; Coffey et al. 2004).”
- Accretion-powered Stellar Winds. II. Numerical Solutions for Stellar Wind Torques (2008, background): “…(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 disk, rather than the star.”
- Disk Surface Density Transitions as Protoplanet Traps (2006, background): “This radius has been inferred to vary from 0.3 to a few AU in some T Tauri stars5 (Coffey et al. 2004; Pesenti et al. 2004).”
- Cavity opening by a giant planet in a protoplanetary disc and effects on planetary migration (2007, background): “…in the case of jet-emitting disc (JED): indeed, at the base of the jet, which may be several astronomical units large (Bacciotti et al. 2003; Coffey et al. 2004), accretion is dominated by the torque exerted by the jet and is much larger than the standard accretion; so, the outer radius of…”
- MHD simulations of jet acceleration from Keplerian accretion disks - The effects of disk resistivity (2007, background): “12), a quantitative comparison with the poloidal speed (Bacciotti et al. 2000) and rotation signatures (Bacciotti et al. 2002; Coffey et al. 2004; Woitas et al. 2005) of the observed outflows is much more difficult, because the size of our computational domain, which reaches a physical scale along…”
- Which jet launching mechanism(s) in T Tauri stars (2006, methodology): “Detections of transverse velocity shifts suggestive of rotati n signatures have been recently derived from HST/STIS spectra at distances≃ 50 AU from the central source in 4 T Tauri microjets: DG Tau, Th 28, LkHα 321, and RW Aur (Bacciotti et al. 2002; Coffey et al. 2004; Woitas et al. 2005).”
- Probing T Tauri Accretion and Outflow with 1 Micron Spectroscopy (2006, background): “An intriguing result comes from spectroscopy at high spatial resolution of T Tauri ”micro jets” revealing velocity asymmetries that have been interpreted as coherent rotation of the jet as would be imparted from an MHD disk wind launched from moderate disk radii of 0.5-2 AU (Coffey et al. 2004).”