2004
DOI: 10.1051/0004-6361:20040033
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Predicted rotation signatures in MHD disc winds and comparison to DG Tau observations

Abstract: Abstract.Motivated by the first detections of rotation signatures in the DG Tau jet , we examine possible biases affecting the relation between detected rotation signatures and true azimuthal velocity for self-similar MHD disc winds, taking into account projection, convolution as well as excitation gradients effects. We find that computed velocity shifts are systematically smaller than the true underlying rotation curve. When outer slower streamlines dominate the emission, we predict observed shifts increasing… Show more

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Cited by 90 publications
(166 citation statements)
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“…If these cones traced actual streamlines, an extrapolation back to the origin would suggest that the HVB component in DG Tau originates in a disk radius <4 AU and the MVB in a disk radius <1 AU. This is compatible with the maximum launch radii of 0.5 AU and 2-3 AU derived from tentative jet rotation signatures at projected flow speeds of -200 km s −1 and -50 km s −1 respectively (Coffey et al 2007;Bacciotti 2002;Pesenti et al 2004). However, it is likely that emission maps in constant velocity bins do not trace actual streamlines especially at low flow velocities.…”
Section: Collimation Opening Angle and Upper Limits On Launch Radiisupporting
confidence: 81%
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“…If these cones traced actual streamlines, an extrapolation back to the origin would suggest that the HVB component in DG Tau originates in a disk radius <4 AU and the MVB in a disk radius <1 AU. This is compatible with the maximum launch radii of 0.5 AU and 2-3 AU derived from tentative jet rotation signatures at projected flow speeds of -200 km s −1 and -50 km s −1 respectively (Coffey et al 2007;Bacciotti 2002;Pesenti et al 2004). However, it is likely that emission maps in constant velocity bins do not trace actual streamlines especially at low flow velocities.…”
Section: Collimation Opening Angle and Upper Limits On Launch Radiisupporting
confidence: 81%
“…Furthermore, the slowest jet material at V r 30−60 km s −1 exhibits velocity shifts between the two sides of the jet (Bacciotti et al 2000;Coffey et al 2007) in the same sense as the rotation of the DG Tau disk (Testi et al 2002). These transverse shifts excellently agree with predicted rotation signatures for a steady-state MHD disk wind launched out to about 3 AU (Anderson et al 2003;Pesenti et al 2004;Ferreira et al 2006). A velocity shift in the same sense is seen across faster jet material at −200 km s −1 suggesting (if caused by rotation) ejection from smaller disk radii of 0.2−0.5 AU (Coffey et al 2007).…”
Section: Introductionsupporting
confidence: 72%
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