2010A&A...516A...6S


Query : 2010A&A...516A...6S

2010A&A...516A...6S - Astronomy and Astrophysics, volume 516, A6-6 (2010/6-2)

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

STUTE M., GRACIA J., TSINGANOS K. and VLAHAKIS N.

Abstract (from CDS):

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. Analytical radially self-similar models successfully describe disk-winds, but need several improvements. 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. This is our main goal. In order to compare our models with observed jet widths inferred from recent optical images taken with the Hubble Space Telescope (HST) and ground-based adaptive optics (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 full-width half-maximum 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. Furthermore, 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 1AU in the observed sample for the considered disk-wind solution. One disk-wind simulation with an inner truncation radius at about 0.11AU also shows potential for reproducing the observations, but a parameter study is needed.

Abstract Copyright:

Journal keyword(s): magnetohydordynamics - methods: numerical - ISM: jets and outflows - stars: pre-main sequence

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* CW Tau TT* 04 14 17.0042670144 +28 10 57.766508508 13.92 13.64 12.36 12.86   K0Ve 344 0
2 V* T Tau TT* 04 21 59.4319873992 +19 32 06.432393336   11.22 10.12 9.80   K0IV/Ve 1373 1
3 V* DG Tau Or* 04 27 04.6921275888 +26 06 16.060169268 13.57 13.97 10.50 12.28   K6Ve 1000 1
4 V* V1213 Tau Or* 04 31 37.5055489536 +18 12 24.383952396           K7 548 0
5 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1361 0
6 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
7 V* UZ Tau B TT* 04 32 42.8118779016 +25 52 31.198173600   14.07 12.72 13.35   M1/3Ve 145 0
8 V* HN Tau Or* 04 33 39.3629421552 +17 51 52.289234280   14.76 13.40 13.05   K5e 245 0
9 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 763 0
10 HH 34 HH 05 35 31.30 -06 28 43.0     16     ~ 479 2

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2023.02.07-15:09:42

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