Herbig-Haro Flows from the L1641-N Embedded Infrared Cluster

Reipurth, Bo; Devine, David; Bally, John

doi:10.1086/300513

Cited by 34 publications

(50 citation statements)

References 26 publications

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“…All 11 new jets have well identified visible driving sources and among those, 7 are included in the Pettersson et al catalog (the rest presumably being fainter than the detection limit of the Pettersson et al survey). One more of the 99 stars of Petterson et al is associated with a jet, HH 305, namely a fainter companion to the young variable PR Ori (Reipurth et al 1998a, also see Fig. 1).…”

Section: How Common Are Jets During the T Tauri Stage?mentioning

confidence: 91%

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Faint Collimated Herbig-Haro Jets From Visible Stars in L1641

Reipurth

Aspin

Bally

et al. 2010

The Astronomical Journal

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A population of 11 faint, collimated jets has been discovered in the northern part of the L1641 cloud in the region of HH 1/2, HH 34, and the L1641-N cluster. These jets were missed in previous imaging surveys on account of their weak emission, and they were discovered only on deep exposures with the Subaru 8m telescope. With these new faint jets, the number of HH flows within the area surveyed has doubled. This suggests that collimated jets from young stars may be more common than assumed so far. It is noteworthy that all of the jets are associated with optically visible stars with r-magnitudes ranging from 13.8 to 22.0. The driving sources of jets in regions flooded by ultraviolet radiation from nearby OB stars are known to be excavated by photo-ionization, and in three cases remnant Hα emission envelopes are found associated with the sources, although the more benign environment in the region observed here, about 10 pc distant from the Orion Nebula Cluster, makes the optical visibility of all these sources rather surprising. Such faint jets from visible stars represent either the final vestiges of the outflow phenomenon, or they are triggered by disturbances of the remnant disks, possibly initiated by the orbital evolution of binaries that spiral in to form close binaries. Among the known Hα emission stars within the region surveyed, 8% are found to be associated with jets.

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Section: How Common Are Jets During the T Tauri Stage?mentioning

confidence: 91%

“…If one follows the well defined flow axis of the HH 1029 flow from the source to the NW one comes to an already known object, HH 298A (Reipurth et al 1998a), located along the flow axis and at the same distance to the source as the first bright knot in the HH 1029 jet. This strongly suggests that HH 298A is a part of the counterflow to HH 1029.…”

Section: Hh 1029mentioning

confidence: 99%

Faint Collimated Herbig-Haro Jets From Visible Stars in L1641

Reipurth

Aspin

Bally

et al. 2010

The Astronomical Journal

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“…For L1641N, there is evidence that the stellar feedback may have dispersed the clump material significantly (Reipurth et al 1998;Nakamura et al 2012). For the intermediate mass clumps such as the Serpens Main Cloud and Serpens South, the outflow kinetic energy may partly influence the clump dynamical evolution.…”

Section: Dynamical Impact Of Outflow Feedbackmentioning

confidence: 99%

Confronting the Outflow-Regulated Cluster Formation Model With Observations

Nakamura

2014

ApJ

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Protostellar outflows have been shown theoretically to be capable of maintaining supersonic turbulence in cluster-forming clumps and keeping the star formation rate per free-fall time as low as a few percent. We aim to test two basic predictions of this outflow-regulated cluster formation model, namely (1) the clump should be close to virial equilibrium and (2) the turbulence dissipation rate should be balanced by the outflow momentum injection rate, using recent outflow surveys toward 8 nearby cluster-forming clumps (B59, L1551, L1641N, Serpens Main Cloud, Serpens South, ρ Oph, IC 348, and NGC 1333). We find, for almost all sources, that the clumps are close to virial equilibrium and the outflow momentum injection rate exceeds the turbulence momentum dissipation rate. In addition, the outflow kinetic energy is significantly smaller than the clump gravitational energy for intermediate and massive clumps with M cl a few × 10 2 M ⊙ , suggesting that the outflow feedback is not enough to disperse the clump as a whole. The number of observed protostars also indicates that the star formation rate per free-fall time is as small as a few percent for all clumps. These observationally-based results strengthen the case for outflow-regulated cluster formation.

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“…1), that the σ Orionis cluster gained in importance. The subsequent detection of Herbig-Haro objects (Reipurth et al 1998), brown dwarfs (Béjar et al 1999), the least massive object directly detected out of the Solar System (S Ori 70; Zapatero Osorio et al 2002b), and planetary-mass objects with discs (Zapatero Osorio et al 2007) have transformed σ Orionis into a cornerstone for the study of stellar and substellar populations in very young open clusters. See Caballero (2007aCaballero ( , 2008c for comprehensive σ Orionis data compilations.…”

Section: Introductionmentioning

confidence: 99%

New deepXMM-Newtonobservations to the west of the σ Orionis cluster

López‐Santiago

Caballero

2008

A&A

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Aims. The objective of this study is to determine the general X-ray properties of the young stars in the external regions of the σ Orionis cluster (τ ∼ 3 Ma, d ∼ 385 pc) and determine constraints on the X-ray emission of brown dwarfs. Methods. We carried out a careful analysis of public data obtained from an unexplored region to the west of the centre of the cluster with the three EPIC cameras onboard the XMM-Newton mission. We looked for new X-ray young stars among the 41 identified X-ray sources in the area with maximum likelihood parameters L > 15 by cross-correlation with the USNO-B1, DENIS, and 2MASS databases.Results. Based on colour-colour, colour-magnitude, and hardness ratio diagrams, and previous spectroscopic, astrometric, and infrared-flux excess information, we classified the optical/near-infrared counterparts of the X-ray sources into: young stars (15), field stars (4), galaxies (19), and sources of unknown nature (3). Most of the X-ray detections, including those of nine young stars, are new. We derived the X-ray properties (e.g. temperatures, metallicities, column densities) of the twelve young stars with the largest signal-to-noise ratios. The X-ray parameters determined here are in good agreement with those found in the cluster centre, where the stellar density is higher. There is no relation between infrared excess and column density in the X-ray measurements in our data. We detected flaring events in two young stars of the sample. One of them showed a very large (∼30) relative increase in flux. Both stars showed high coronal temperatures during the observation. Finally, we determined upper limits to the flux of the young stars and brown dwarfs not detected by our search algorithm.

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Herbig-Haro Flows from the L1641-N Embedded Infrared Cluster

Cited by 34 publications

References 26 publications

Faint Collimated Herbig-Haro Jets From Visible Stars in L1641

Faint Collimated Herbig-Haro Jets From Visible Stars in L1641

Confronting the Outflow-Regulated Cluster Formation Model With Observations

New deepXMM-Newtonobservations to the west of the σ Orionis cluster

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