2015A&A...581A..85P


Query : 2015A&A...581A..85P

2015A&A...581A..85P - Astronomy and Astrophysics, volume 581A, 85-85 (2015/9-1)

The jet and the disk of the HH 212 low-mass protostar. imaged by ALMA: SO and SO2 emission.

PODIO L., CODELLA C., GUETH F., CABRIT S., BACHILLER R., GUSDORF A., LEE C.-F., LEFLOCH B., LEURINI S., NISINI B. and TAFALLA M.

Abstract (from CDS):

The investigation of the disk formation and jet launching mechanism in protostars is crucial to understanding the earliest stages of star and planet formation. We aim to constrain the physical and dynamical properties of the molecular jet and disk of the HH 212 protostellar system at unprecedented angular scales, exploiting the capabilities of the Atacama Large Millimeter Array (ALMA). The ALMA observations of HH 212 in emission lines from sulfur-bearing molecules, SO 98-87, SO 1011-1010, SO2 82,6-71,7, are compared with simultaneous CO 3-2, SiO 8-7 data. The molecules column density and abundance are estimated using simple radiative transfer models. SO 98-87 and SO2 82,6-71,7 show broad velocity profiles. At systemic velocity, they probe the circumstellar gas and the cavity walls. Going from low to high blue- and red-shifted velocities the emission traces the wide-angle outflow and the fast (∼100-200km/s), collimated (∼90AU) molecular jet revealing the inner knots with timescales ≤50yr. The jet transports a mass-loss rate ≥0.2-2x10–6M/yr, implying high ejection efficiency (≥0.03-0.3). The SO and SO2 abundances in the jet are ∼10–7-10–6. SO 1011-1010 emission is compact and shows small-scale velocity gradients, indicating that it originates partly from the rotating disk previously seen in HCO+ and C17O, and partly from the base of the jet. The disk mass is ≥0.002-0.013M and the SO abundance in the disk is ∼10–8-10–7. SO and SO2 are effective tracers of the molecular jet in the inner few hundreds AU from the protostar. Their abundances indicate that 1-40% of sulfur is in SO and SO2 due to shocks in the jet/outflow and/or to ambipolar diffusion at the wind base. The SO abundance in the disk is 3-4 orders of magnitude larger than in evolved protoplanetary disks. This may be due to an SO enhancement in the accretion shock at the envelope-disk interface or in spiral shocks if the disk is partly gravitationally unstable.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: jets and outflows - ISM: molecules - ISM: individual objects: HH 212

CDS comments: Figure 1, Table 2 knots not in SIMBAD.

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 - 2023
#notes
1 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 325 0
2 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 436 3
3 [JCC87] IRAS 4A2 Y*O 03 29 10.413 +31 13 32.20           ~ 106 1
4 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1357 1
5 HH 211 Y*O 03 43 56.52 +32 00 52.8           ~ 342 0
6 IRAS 04166+2706 Y*O 04 19 42.62736 +27 13 38.4312           ~ 127 0
7 IRAS 04302+2247 Y*O 04 33 16.50096 +22 53 20.4000           ~ 161 0
8 LDN 1527 DNe 04 39 53 +25 45.0           ~ 581 0
9 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1006 2
10 QSO B0537-441 BLL 05 38 50.36155950 -44 05 08.9390233   15.77 16.48 16   ~ 847 2
11 [CCG2007] MM1 smm 05 43 51.4100 -01 02 53.160           ~ 16 1
12 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 350 1
13 QSO B0605-0834 BLL 06 07 59.69924014 -08 34 49.9783246     18.5 17.70   ~ 425 1
14 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 399 0
15 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 549 0

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2022.12.07-05:34:27

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