Rotating molecular outflows: the young T Tauri star in CB 26

Launhardt, R.; Pavlyuchenkov, Ya. N.; Gueth, F.; Chen, X.; Dutrey, Anne; Guilloteau, S.; Henning, Th.; Piétu, V.; Schreyer, K.; Semenov, D.

doi:10.1051/0004-6361:200810835

Cited by 90 publications

(158 citation statements)

References 35 publications

(61 reference statements)

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“…The molecular region will move even further out in Class II sources. This predicted trend is in line with possible rotation signatures reported so far in molecular Class I/II jets (HH26 and CB26), which do appear to suggest larger magnetocentrifugal launch radii 3−10 AU than in Class 0 jets, although statistics are admittedly still limited (Chrysostomou et al 2008;Launhardt et al 2009;Cabrit 2009). This prediction also seems promising to explain the trend towards slow, wide molecular counterparts in older Class II jet sources.…”

Section: Predicted Observational Trends and Future Testssupporting

confidence: 88%

Molecule survival in magnetized protostellar disk winds

Panoglou¹,

Cabrit²,

Forêts³

et al. 2012

A&A

101

144

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Context. Molecular counterparts to atomic jets have recently been detected within 1000 AU of young stars at early evolutionary stages. Reproducing these counterparts is an important new challenge for proposed ejection models. Aims. We explore whether molecules may survive in the magneto-hydrodynamic (MHD) disk wind solution currently invoked to reproduce the kinematics and tentative rotation signatures of atomic jets in T Tauri stars. Methods. The coupled ionization, chemical, and thermal evolution along dusty flow streamlines is computed for the prescribed MHD disk wind solution, using a method developed for magnetized shocks in the interstellar medium. Irradiation by (wind-attenuated) coronal X-rays and far-ultraviolet photons from accretion hot spots is included, with an approximate self-shielding of H 2 and CO. Disk accretion rates of 5 × 10 −6 , 10 −6 and 10 −7 M yr −1 are considered, representative of low-mass young protostars (so-called "Class 0"), evolved protostars ("Class I") and very active T Tauri stars ("Class II") respectively. Results. The disk wind has an "onion-like" thermo-chemical structure, with streamlines launched from larger radii having lower temperature and ionization, and higher H 2 abundance. The coupling between charged and neutral fluids is sufficient to eject molecules from the disk out to at least 9 AU. The launch radius beyond which most H 2 survives moves outward with evolutionary stage, from 0.2 AU (sublimation radius) in the Class 0 disk wind, to 1 AU in the Class I, and >1 AU in the Class II. In this molecular wind region, CO survives in the Class 0 but is significantly photodissociated in the Class I/II. Balance between ambipolar heating and molecular cooling establishes a moderate asymptotic temperature 700−3000 K, with cooler jets at earlier protostellar stages. As a result, endothermic formation of H 2 O is efficient, with abundances up to 10 −4 , while CH + and SH + can reach ≥10 −6 in the hotter and more ionised Class I/II winds. Conclusions. A centrifugal MHD disk wind launched from beyond 0.2−1 AU can produce molecular jets/winds up to speeds 100 km s −1 in young low-mass stars ranging from Class 0 to active Class II. The model predicts a high abundance ratio of H 2 to CO and an increase of molecular launch radius, temperature, and flow width as the source evolves, in promising agreement with current observed trends. Calculations of synthetic maps and line profiles in H 2 , CO and H 2 O will allow detailed tests of the model against observations.

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Section: Predicted Observational Trends and Future Testssupporting

confidence: 88%

Molecule survival in magnetized protostellar disk winds

Panoglou¹,

Cabrit²,

Forêts³

et al. 2012

A&A

101

144

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“…There are some interpretations of this velocity gradient, and one of these is a rotating outflow. The rotations of the outflows in CO observations were reported in the Class-I and II sources (e.g., Launhardt et al 2009;Pech et al 2012). The velocity structure in the northeastern lobe of the B59#11 outflow is very similar to those in outflows ejected from the Class-II YSO CB26 (Launhardt et al 2009) and the Class-I YSO HH797 (Pech et al 2012), two very reliable candidates for a rotating molecular outflow.…”

Section: A Rotating Outflow In B59#11?mentioning

confidence: 74%

The Rotating Outflow, Envelope, and Disk of the Class-0/I Protostar [Bhb2007]#11 in the Pipe Nebula

Hara

Shimajiri

Tsukagoshi

et al. 2013

ApJ

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We present the results of observations toward a low-mass Class-0/I protostar [BHB2007]#11 (B59#11) in the nearby (d = 130 pc) star-forming region Barnard 59 (B59), in the Pipe Nebula. We utilize the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope (∼22 resolution), focusing on the CO(3-2), HCO + , H 13 CO + (4-3), and 1.1 mm dust-continuum emission transitions. We also show Submillimeter Array (SMA) data with ∼5 resolution in 12 CO, 13 CO, C 18 O(2-1), and 1.3 mm dust-continuum emission. From ASTE CO(3-2) observations, we found that B59#11 is blowing a collimated outflow whose axis lies almost on the plane of the sky. The outflow traces well a cavity-like structure seen in the 1.1 mm dust-continuum emission. The results of SMA 13 CO and C 18 O(2-1) observations have revealed that a compact and elongated structure of dense gas is associated with B59#11; the structure is oriented perpendicular to the outflow axis. There is a compact dust condensation with a size of 350 × 180 AU seen in the SMA 1.3 mm continuum map, and the direction of its major axis is almost the same as that of the dense gas elongation. The distributions of 13 CO and C 18 O emission also show velocity gradients along their major axes, which are thought to arise from the envelope/disk rotation. From detailed analysis of the SMA data, we infer that B59#11 is surrounded by a Keplerian disk with a radius of less than 350 AU. In addition, the SMA CO(2-1) image shows a velocity gradient in the outflow in the same direction as that of the dense gas rotation. We suggest that this velocity gradient indicates rotation in the outflow.

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“…CB26 is a deeply embedded, edge-on object driving an unusual outflow (Launhardt et al 2009) in an isolated Bok globule. Like in HL Tau, we detect here strong H 2 CO and SO emission, but only a weak CN line.…”

Section: Discussionmentioning

confidence: 99%

A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars

Guilloteau¹,

Folco²,

Dutrey³

et al. 2013

A&A

Self Cite

104

151

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Aims. We investigate the suitability of several molecular tracers, in particular CN N = 2−1 line emission, as a confusion-free probe of the kinematics of circumstellar disks. Methods. We use the IRAM 30-m telescope to perform a sensitive search for CN N = 2−1 in 42 T Tauri or Herbig Ae systems located principally in the Taurus-Auriga region. 13 CO J = 2−1 is observed simultaneously to provide an indication of the level of confusion with the surrounding molecular cloud. The bandpass also contains two transitions of ortho-H 2 CO, one of SO and the C 17 O J = 2−1 line which provide complementary information on the nature of the emission. Results. While 13 CO is in general dominated by residual emission from the cloud, CN exhibits a high disk detection rate >50% in our sample. We even report CN detection in stars for which interferometric searches failed to detect 12 CO, presumably because of obscuration by a foreground, optically thick, cloud. Comparison between CN and o-H 2 CO or SO line profiles and intensities divide the sample in two main categories. Sources with SO emission are bright and have strong H 2 CO emission, leading in general to [H 2 CO/CN] > 0.5. Furthermore, their line profiles, combined with a priori information on the objects, suggest that the emission is coming from outflows or envelopes rather than from a circumstellar disk. On the other hand, most sources have [H 2 CO/CN] < 0.3, no SO emission, and some of them exhibit clear double-peaked profiles characteristics of rotating disks. In this second category, CN is likely tracing the proto-planetary disks. From the line flux and opacity derived from the hyperfine ratios, we constrain the outer radii of the disks, which range from 300 to 600 AU. The overall gas disk detection rate (including all molecular tracers) is ∼68%, and decreases for fainter continuum sources. Conclusions. The current study demonstrates that gas disks, like dust disks, are ubiquitous around young PMS stars in regions of isolated star formation, and that a large fraction of them have R out > ∼ 300 AU. It also shows the potential of the CN N = 2−1 transition to probe the kinematics of these disks, thereby measuring the stellar mass, using high resolution observations with ALMA.

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Rotating molecular outflows: the young T Tauri star in CB 26

Cited by 90 publications

References 35 publications

Molecule survival in magnetized protostellar disk winds

Molecule survival in magnetized protostellar disk winds

The Rotating Outflow, Envelope, and Disk of the Class-0/I Protostar [Bhb2007]#11 in the Pipe Nebula

A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars

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Rotating molecular outflows: the young T Tauri star in CB 26

Cited by 90 publications

References 35 publications

Molecule survival in magnetized protostellar disk winds

Molecule survival in magnetized protostellar disk winds

The Rotating Outflow, Envelope, and Disk of the Class-0/I Protostar [Bhb2007]#11 in the Pipe Nebula

A sensitive survey for13CO, CN, H2CO, and SO in the disks of T Tauri and Herbig Ae stars

Contact Info

Product

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A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars