2019A&A...623A..96Y


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.26CEST21:24:19

2019A&A...623A..96Y - Astronomy and Astrophysics, volume 623A, 96-96 (2019/3-1)

Signs of outflow feedback from a nearby young stellar object on the protostellar envelope around HL Tauri.

YEN H.-W., TAKAKUWA S., GU P.-G., HIRANO N., LEE C.-F., LIU H.B., LIU S.-Y. and WU C.-J.

Abstract (from CDS):


Aims. HL Tau is a Class I-II protostar embedded in an infalling and rotating envelope and possibly associated with a planet forming disk, and it is co-located in a 0.1pc molecular cloud with two nearby young stellar objects with projected distance of ∼20''-30'' (2800-4200au) to HL Tau. Our observations with the Atacama Large Millimeter/Submillimeter Array (ALMA) revealed two arc-like structures on a 1000au scale connected to the disk, and their kinematics could not be explained with any conventional model of infalling and rotational motions. In this work, we investigate the nature of these arc-like structures connected to the HL Tau disk.
Methods. We carried out new observations in the 13CO and C18O (3-2; 2-1) lines with the James Clerk Maxwell Telescope and the IRAM 30m telescope, and obtained the data with the 7-m array of the Atacama Compact Array (ACA). With the single-dish, ACA, and ALMA data, we analyzed the gas motions on both 0.1pc and 1000au scales in the HL Tau region. We constructed new kinematical models of an infalling and rotating envelope with the consideration of relative motion between HL Tau and the envelope.
Results. By including the relative motion between HL Tau and its protostellar envelope, our kinematical model can explain the observed velocity features in the arc-like structures. The morphologies of the arc-like structures can also be explained with an asymmetric initial density distribution in our model envelope. In addition, our single-dish results support the scenario that HL Tau is located at the edge of a largescale (0.1pc) expanding shell driven by the wind or outflow from XZ Tau, as suggested in the literature. The estimated expanding velocity of the shell is comparable to the relative velocity between HL Tau and its envelope in our kinematical model. These results hint that the largescale expanding motion likely impacts the protostellar envelope around HL Tau and affects its gas kinematics. We found that the mass infalling rate from the envelope onto the HL Tau disk can be decreased by a factor of two due to this impact by the largescale expanding shell.

Abstract Copyright: © ESO 2019

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

Status at CDS:  

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 LDN 1448 DNe 03 22.5 +30 35           ~ 463 0
2 NAME LDN 1448-mm Y*O 03 25 38.83 +30 44 06.2           ~ 299 0
3 RAFGL 5123 FU* 04 31 34.07736 +18 08 04.9020           K3V/M3III 806 0
4 EM* LkHA 358 TT* 04 31 36.1396524070 +18 13 43.176961457     19.0     M0.9 86 0
5 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1186 0
6 V* XZ Tau Or* 04 31 40.0868968022 +18 13 56.642439056     10.40 13.12   M2e+M2e 406 1
7 2MASS J04314444+1808315 Y*O 04 31 44.44680 +18 08 31.5384           ~ 149 0
8 QSO J0431+1731 BLL 04 31 57.37922 +17 31 35.7762       21.3   ~ 33 1
9 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3443 0
10 QSO B0507+179 QSO 05 10 02.36912982 +18 00 41.5816534   20.0 19.0 19.09   ~ 307 1
11 QSO B0521-365 BLL 05 22 57.9839686440 -36 27 30.847737786   15.26 14.62 14.48   ~ 707 2
12 NAME Ori A MoC 05 38 -07.1           ~ 2663 0

    Equat.    Gal    SGal    Ecl

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2020.05.26-21:24:19

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