Comparison of synthetic maps from truncated jet-formation models with YSO jet observations

Abstract

(abridged) Significant progress has been made in the last years in the understanding of the jet formation mechanism through a combination of numerical simulations and analytical MHD models for outflows characterized by the symmetry of self-similarity. In a previous article we introduced models of truncated jets from disks, i.e. evolved in time numerical simulations based on a radially self-similar MHD solution, but including the effects of a finite radius of the jet-emitting disk and thus the outflow. These models need now to be compared with available observational data. A direct comparison of the results of combined analytical theoretical models and numerical simulations with observations has not been performed as yet. In order to compare our models with observed jet widths inferred from recent optical images taken with HST and AO observations, we use a new set of tools to create emission maps in different forbidden lines, from which we determine the jet width as the FWHM of the emission. It is shown that the untruncated analytical disk outflow solution considered here cannot fit the small jet widths inferred by observations of several jets. Various truncated disk-wind models are examined, whose extracted jet widths range from higher to lower values compared to the observations. Thus we can fit the observed range of jet widths by tuning our models. We conclude that truncation is necessary to reproduce the observed jet widths and our simulations limit the possible range of truncation radii. We infer that the truncation radius, which is the radius on the disk mid-plane where the jet-emitting disk switches to a standard disk, must be between around 0.1 up to about 1 AU in the observed sample for the considered disk-wind solution. One disk-wind simulation with an inner truncation radius at about 0.11 AU also shows potential for reproducing the observations, but a parameter study is needed.

accepted for publication in A & A, 14 pages, 21 figures

References in corpus (5)

• PLUTO: a Numerical Code for Computational Astrophysics
• MHD simulations of jet acceleration from Keplerian accretion disks: the effects of disk resistivity
• Two-component jet simulations: I. Topological stability of analytical MHD outflow solutions
• Two-component jet simulations: II. Combining analytical disk and stellar MHD outflow solutions
• Stability and structure of analytical MHD jet formation models with a finite outer disk radius

Cited by in corpus (5)

• Protostellar Outflows and Radiative Feedback from Massive Stars. II. Feedback, Star Formation Efficiency, and Outflow Broadening
• Confronting 3 Dimensional Time-dependent Jet Simulations with HST Observations
• Young stellar object jet models: From theory to synthetic observations
• 3D simulations of disc-winds extending radially self-similar MHD models
• Comparison of synthetic maps from truncated jet-formation models with YSO jet observations. II. The effect of varying inclinations