3-D numerical simulations of rotating jets: The case of the DG Tau microjet

Abstract

We here present results of three-dimensional Smoothed Particle hydro and magnetohydrodynamics simulations of rotating jets, also including the effects of radiative cooling, precession and velocity variability. Using initial conditions and parameters which are particularly suitable for the DG Tau microjet, we have been able to approximately reproduce its complex knotty morphology and kinematics. We have also obtained radial velocity maps which are in good agreement with the data obtained by Bacciotti et al., thus indicating that their interpretation that the DG Tau microjet is rotating is correct. Finally, we have found that a magnetic field of the order of ~ 0.5 mG is sufficient to collimate the jet against the lateral expansion that is caused by the centrifugal forces.

arXiv comment4 pages, 3 figures; Accepted for publication in A&A (letters). The high resolution figures are avilable upon request

References in corpus (6)

• HST/STIS Spectroscopy of the Optical Outflow from DG Tau: Indications for Rotation in the Initial Jet Channel
• Rotation of Jets from Young Stars: New Clues from the Hubble Space Telescope Imaging Spectrograph
• Predicted rotation signatures in MHD disc winds and comparison to DG Tau observations
• The precession of the giant HH34 outflow: a possible jet deceleration mechanism
• Three-dimensional MHD simulations of Radiatively cooling, Pulsed Jets
• The deceleration of Giant Herbig-Haro Flows

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• Time Variability of Emission Lines for Four Active T Tauri Stars (I): October--December in 2010
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• Transverse velocity shifts in protostellar jets: rotation or velocity asymmetries?
• Proper motions of radiative knots in simulations of stellar jets - An alternative to pulsating inflow conditions
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