2017A&A...608A.134Y


Query : 2017A&A...608A.134Y

2017A&A...608A.134Y - Astronomy and Astrophysics, volume 608A, 134-134 (2017/12-1)

1000 au exterior arcs connected to the protoplanetary disk around HL Tauri.

YEN H.-W., TAKAKUWA S., CHU Y.-H., HIRANO N., HO P.T.P., KANAGAWA K.D., LEE C.-F., LIU H.B., LIU S.-Y., MATSUMOTO T., MATSUSHITA S., MUTO T., SAIGO K., TANG Y.-W., TREJO A. and WU C.-J.

Abstract (from CDS):

Aims. The protoplanetary disk around HL Tau is the youngest candidate of planet formation known to date, and it is still embedded in a protostellar envelope with a size of thousands of au. In this work, we study the gas kinematics in the envelope and its possible influence on the embedded disk.
Methods. We present our new ALMA cycle 3 observational results of HL Tau in the 13CO (2-1) and C18O (2-1) emission at resolutions of 0.8 (110au), and we compare the observed velocity pattern with models of different types of gas motion.
Results. The 13CO and C18O emission lines both show a central compact component with a size of 2'' (280au) that traces the protoplanetary disk. The disk is clearly resolved and shows Keplerian motion, based on which, the protostellar mass of HL Tau is estimated to be 1.8±0.3M, assuming the inclination angle of the disk to be 47° from the plane of the sky. The 13CO emission shows two arc structures with sizes of 1000-2000au and masses of 3x10–3M connected to the central disk. One is blueshifted and stretches from the northeast to the northwest, and the other is redshifted and stretches from the southwest to the southeast. We find that simple kinematical models of infalling and (counter-)rotating flattened envelopes cannot fully explain the observed velocity patterns in the arc structures. The gas kinematics of the arc structures can be better explained with three-dimensional infalling or outflowing motions. Nevertheless, the observed velocity in the northwestern part of the blueshifted arc structure is ∼60-70% higher than the expected free-fall velocity. We discuss two possible origins of the arc structures: (1) infalling flows externally compressed by an expanding shell driven by XZ Tau; and (2) outflowing gas clumps caused by gravitational instabilities in the protoplanetary disk around HL Tau.

Abstract Copyright: © ESO, 2017

Journal keyword(s): protoplanetary disks - stars: formation - ISM: kinematics and dynamics - ISM: kinematics and dynamics

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 IRAS 04016+2610 Y*O 04 04 43.07064 +26 18 56.3904           ~ 246 0
2 LDN 1489 DNe 04 04 47.5 +26 19 42           ~ 211 0
3 PKS 0428+205 rG 04 31 03.7614907 +20 37 34.264207   22.174   19.085   ~ 177 1
4 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1319 0
5 V* XZ Tau Or* 04 31 40.0868968022 +18 13 56.642439056     10.40 13.12   M2e+M2e 423 1
6 IRAS 04365+2535 Y*O 04 39 35.19360 +25 41 44.7252           ~ 260 0
7 LDN 1527 DNe 04 39 53 +25 45.0           ~ 562 0
8 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3926 0
9 QSO B0507+179 QSO 05 10 02.3689932504 +18 00 41.582562768   20.0 19.0 19.09   ~ 370 1
10 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1736 1
11 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1158 1

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2022.05.28-23:19:21

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