CO Outflows from Young Stars: Confronting the Jet and Wind Models

Lee, Chin-Fei; Mundy, Lee G.; Reipurth, Bo; Ostriker, Eve C.; Stone, James M.

doi:10.1086/317056

Cited by 208 publications

(314 citation statements)

References 45 publications

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“…Note the large image scale employed in which a long CO tail is exhibited. The two panels are comparable to the CO map and P-V diagrams of Lee et al (2000), where the large tailed bow was found associated with HH 240A. More blue emission, however, is observed to be associated with the southern wing, not predicted here.…”

Section: Co Structuresupporting

confidence: 80%

“…In the east, however, there is also ample blueshifted CO gas. Lee et al (2000) favour a jet-driven model with a jet orientation of 30 • -60 • to the line of sight.…”

Section: Introductionmentioning

confidence: 88%

“…A large volume of swept up and disturbed gas, however, may still be observable at longer wavelengths through emission in CO rotational transitions, and other molecules. An excellent example of this is associated with the L1634 cloud (Lee et al 2000). We present here a detailed study of the HH objects in L1634 which possess a particularly striking morphology.…”

Section: Introductionmentioning

confidence: 91%

“…CO imaging and spectroscopy in the J = (1, 0) line of the L1634 outflow have been presented by Lee et al (2000). They demonstrated that cold gas in motion is associated with HH 240A, where it curves around with the H 2 shape.…”

Section: Co Structurementioning

confidence: 98%

“…The blue emission curves around the giant HH 240A bow shock with a broad range of radial velocities (including some red-shifted) but there is very little CO emission beyond this location (Lee et al 2000). The CO red wing emission to the east takes the form of a hollow shell which ends near the cloud edge (Lee et al 2000).…”

Section: Introductionmentioning

confidence: 97%

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A near-infrared study of the bow shocks within the L1634 protostellar outflow

O’Connell

Smith

Davis

et al. 2004

A&A

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Abstract. The L1634 bright-rimmed globule contains an intriguing arrangement of shock structures: two series of aligned molecular shock waves associated with the Herbig-Haro flows HH 240 and HH 241. We present near-infrared spectroscopy and narrow-band imaging in the (1, 0) S(1) and (2, 1) S(1) emission lines of molecular hydrogen. These observations yield the spatial distributions of both the molecular excitation and velocity, which demonstrate distinct properties for the individual bow shocks. Bow shock models are applied, varying the shock physics, geometry, speed, density and magnetic field properties to fit two prominent bow shocks. The models predict that both bows move at 60 • to the plane of the sky. High magnetic fields and low molecular fractions are implied. The advancing compact bow HH 240C is interpreted as a J-type bow (frozen-in magnetic field) with the flanks in transition to C-type (field diffusion). It is a paraboloidal bow of speed ∼42 km s −1 entering a medium of quite high density (2 × 10 4 cm −3 ). The following bow HH 240A is faster despite a lower excitation, moving through a lower density medium. We find a C-type bow shock model to fit all the data for HH 240A. The favoured bow models are then tested comprehensively against published H 2 emission line fluxes and CO spectroscopy. We conclude that, while the CO emission originates from cloud gas directly set in motion, the H 2 emission is generated from shocks sweeping through an outflow. Also considering optical data, we arrive at a global outflow model involving episodic slow-precessing twin jets.

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Section: Co Structuresupporting

confidence: 80%

“…In the east, however, there is also ample blueshifted CO gas. Lee et al (2000) favour a jet-driven model with a jet orientation of 30 • -60 • to the line of sight.…”

Section: Introductionmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 91%

Section: Co Structurementioning

confidence: 98%

Section: Introductionmentioning

confidence: 97%

See 3 more Smart Citations

A near-infrared study of the bow shocks within the L1634 protostellar outflow

O’Connell

Smith

Davis

et al. 2004

A&A

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Outflows in Regions of Star Formation

Liseau¹

High Resolution Infrared Spectroscopy in Astronomy

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Abstract. The high spatial and spectral resolution offered by the new generation of infrared spectrometers at ESO is optimally suited for the observational study of outflows from young stellar objects. Models of interstellar shock waves would benefit from observations of spectrally resolved line profiles. This applies also to attempts of measuring the rotation rates of jets very close to their driving source, which in general suffer considerable extinction. Observations of forbidden lines of ionised iron, [Fe II], could be used to accomplish this. The possibility of using rotational lines of molecular hydrogen, H2, to study the temporal evolution of outflow and disk gas is discussed. Similarly, high resolution IR observations of fluorescent water lines, H2O, open up the possibility to access outflow and disk water from the ground.

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Magnetic Fields in Astrophysical Jets: From Launch to Termination

Hardcastle¹,

Gabuzda²

2012

Space Sciences Series of ISSI

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Long-lived, stable jets are observed in a wide variety of systems, from protostars, through Galactic compact objects to active galactic nuclei (AGN). Magnetic fields play a central role in launching, accelerating, and collimating the jets through various media. The termination of jets in molecular clouds or the interstellar medium deposits enormous amounts of mechanical energy and momentum, and their interactions with the external medium, as well, in many cases, as the radiation processes by which they are observed, are intimately connected with the magnetic fields they carry. This review focuses on the properties and structures of magnetic fields in long-lived jets, from their launch from rotating magnetized young stars, black holes, and their accretion discs, to termination and beyond. We compare the results of theory, numerical simulations, and observations of these diverse systems and address similarities and differences between relativistic and non-relativistic jets in protostellar versus AGN systems. On the observational side, we focus primarily on jets driven by AGN because of the strong observational constraints on their magnetic field properties, and we discuss the links between the physics of these jets on all scales.

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CO Outflows from Young Stars: Confronting the Jet and Wind Models

Cited by 208 publications

References 45 publications

A near-infrared study of the bow shocks within the L1634 protostellar outflow

A near-infrared study of the bow shocks within the L1634 protostellar outflow

Outflows in Regions of Star Formation

Magnetic Fields in Astrophysical Jets: From Launch to Termination

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