2021A&A...650A..46E


Query : 2021A&A...650A..46E

2021A&A...650A..46E - Astronomy and Astrophysics, volume 650A, 46-46 (2021/6-1)

Launching the asymmetric bipolar jet of DO Tau.

ERKAL J., DOUGADOS C., COFFEY D., CABRIT S., BACCIOTTI F., GARCIA-LOPEZ R., FEDELE D. and CHRYSOSTOMOU A.

Abstract (from CDS):


Context. The role of bipolar jets in the formation of stars, and in particular how they are launched, is still not well understood.
Aims. We probe the protostellar jet launching mechanism using high-resolution observations of the near-infrared (IR) [FeII]λ1.53,1.64 µm emission lines.
Methods. We consider the case of the bipolar jet from Classical T Tauri star, DO Tau, and investigate the jet morphology and kinematics close to the star (within 140au) using AO-assisted IFU observations from GEMINI/NIFS.
Results. We find that the brighter, blueshifted jet is collimated very quickly after it is launched. This early collimation requires the presence of magnetic fields. We confirm velocity asymmetries between the two lobes of the bipolar jet, and also confirm no time variability in the asymmetry over a 20-year interval. This sustained asymmetry is in accordance with recent simulations of magnetised disc winds. We examine the data for signatures of jet rotation. We report an upper limit on differences in radial velocity of 6.3 and 8.7km/s for the blue- and redshifted jets, respectively. Interpreting this as an upper limit on jet rotation implies that any steady, axisymmetric magneto-centrifugal model of jet launching is constrained to a launch radius in the disc plane of r0<0.5 and 0.3au for the blue- and redshifted jets, respectively. This supports an X-wind or narrow disc-wind model. However, the result pertains only to the observed high-velocity [FeII] emission, and does not rule out a wider flow launched from a wider radius. We report the detection of small-amplitude jet axis wiggling in both lobes. We rule out orbital motion of the jet source as the cause. Precession can better account for the observations but requires double the precession angle, and a different phase for the counter-jet. Such non-solid body precession could arise from an inclined massive Jupiter companion, or a warping instability induced by launching a magnetic disc wind.
Conclusions. Overall, our observations are consistent with an origin of the DO Tau jets from the inner regions of the disc.

Abstract Copyright: © ESO 2021

Journal keyword(s): ISM: jets and outflows - stars: low-mass - stars: pre-main sequence - ISM: individual objects: DO Tau

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 701 1
2 [EM98] DG Tau B cRN Y*O 04 27 02.66088 +26 05 30.4548           ~ 175 0
3 V* DG Tau Or* 04 27 04.6921275888 +26 06 16.060169268 13.57 13.97 10.50 12.28   K6Ve 1020 1
4 V* V1213 Tau Or* 04 31 37.5055489536 +18 12 24.383952396           K7 564 0
5 V* DO Tau Or* 04 38 28.5880527336 +26 10 49.467596196 12.78 13.44 12.30 13.01   M1Ve 372 1
6 V* HV Tau Or* 04 38 35.2904827968 +26 10 38.640143136           M1Ve 141 0
7 HH 832 HH 04 39 02.0 +26 12 21           ~ 3 0
8 HH 831A HH 04 39 13.2 +26 13 48           ~ 3 0
9 HH 831B HH 04 39 15.2 +26 13 55           ~ 4 0
10 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4373 0
11 V* DP Tau Or* 04 42 37.6989071232 +25 15 36.983641716 15.84 15.2 13.70 14.42   M0.8 172 1
12 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 778 0
13 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 386 1
14 HH 24 HH 05 46 09 -00 10.2           ~ 160 1
15 V* Z CMa Ae* 07 03 43.1599411656 -11 33 06.209065836 10.51 9.99 8.80     B5/8eq+F5/7 575 3

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