Close encounters of the protostellar kind in IC 1396N

Beltrán, M. T.; Massi, F.; Fontani, F.; Codella, C.; López, R.

doi:10.1051/0004-6361/201219166

Cited by 10 publications

(34 citation statements)

References 16 publications

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“…3 panel A). These higher temperatures can result from various heating processes: (i) feedback from low-mass stars, e. g., molecular outflows, as found in some cores of AFGL 5142 or 20293+5932 (e. g., Zhang et al 2002;Palau et al 2007b); (ii) shocks from convergent flows (e. g., Csengeri et al 2011a;Beltrán et al 2012); (iii) feedback from high-mass stars, e. g., strong radiation (e. g., Li et al 2003). In the following, we…”

Section: Temperature Of the Gas And Ir Radiationmentioning

confidence: 99%

Properties of dense cores in clustered massive star-forming regions at high angular resolution

Sánchez-Monge¹,

Palau²,

Fontani³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We aim at characterising dense cores in the clustered environments associated with intermediate/high-mass star-forming regions. For this, we present an uniform analysis of Very Large Array NH 3 (1,1) and (2,2) observations towards a sample of 15 intermediate/high-mass star-forming regions, where we identify a total of 73 cores, classify them as protostellar, quiescent starless, or perturbed starless, and derive some physical properties. The average sizes and ammonia column densities of the total sample are ∼ 0.06 pc and ∼ 10 15 cm −2 , respectively, with no significant differences between the starless and protostellar cores, while the linewidth and rotational temperature of quiescent starless cores are smaller, ∼ 1.0 km s −1 and 16 K, than linewidths and temperatures of protostellar (∼ 1.8 km s −1 and 21 K), and perturbed starless (∼ 1.4 km s −1 and 19 K) cores. Such linewidths and temperatures for these quiescent starless cores in the surroundings of intermediate/high-mass stars are still significantly larger than the typical linewidths and rotational temperatures measured in starless cores of low-mass star-forming regions, implying an important non-thermal component. We confirm at high angular resolutions (spatial scales ∼ 0.05 pc) the correlations previously found with single-dish telescopes (spatial scales 0.1 pc) between the linewidth and the rotational temperature of the cores, as well as between the rotational temperature and the linewidth with respect to the bolometric luminosity. In addition, we find a correlation between the temperature of each core and the incident flux from the most massive star in the cluster, suggesting that the large temperatures measured in the starless cores of our sample could be due to heating from the nearby massive star. A simple virial equilibrium analysis seems to suggest a scenario of a self-similar, self-graviting, turbulent, virialised hierarchy of structures from clumps (∼ 0.1-10 pc) to cores (∼ 0.05 pc). A closer inspection of the dynamical state taking into account external pressure effects, reveal that relatively strong magnetic field support may be needed to stabilise the cores, or that they are unstable and thus on the verge of collapse.

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Section: Temperature Of the Gas And Ir Radiationmentioning

confidence: 99%

Properties of dense cores in clustered massive star-forming regions at high angular resolution

Sánchez-Monge¹,

Palau²,

Fontani³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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“…where R and L are the radius and length of the outflow, respectively, and n * the number density of stars. Beltrán et al (2012) already detected an encounter between two molecular outflows in the star-forming region IC 1396N. They calculated a probability of encounter of two outflows in this cluster of 5% (P ∼0.05).…”

Section: Effects Of Outflow Collisionsmentioning

confidence: 99%

“…At optical wavelengths, the features produced when the ejected material from the stars collide with the surrounding gas and dust are known as Herbig-Haro (HH) objects. At longer wavelengths, the outflows are traced by the emission from different molecules (Arce et al 2007;Beuther et al 2007;Zapata et al 2010;Beltrán et al 2012).…”

Section: Introductionmentioning

confidence: 99%

X-ray embedded stars as driving sources of outflow-driven turbulence in OMC1-S

Rivilla

Martı́n-Pintado

Sanz-Forcada

et al. 2013

Monthly Notices of the Royal Astronomical Society

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Outflows arising from very young stars affect their surroundings and influence the star formation in the parental core. Multiple molecular outflows and Herbig-Haro (HH) objects have been observed in Orion, many of them originating from the embedded massive star-forming region known as OMC1-S. The detection of the outflow driving sources is commonly difficult, because they are still hidden behind large extinction, preventing their direct observation at optical and even near and mid-IR wavelengths. With the aim of improving the identification of the driving sources of the multiple outflows detected in OMC1-S, we used the catalog provided by deep X-ray observations, which have unveiled the very embedded population of pre-main sequence stars. We compared the position of stars observed by the Chandra Orion Ultra Deep project (COUP) in OMC1-S with the morphology of the molecular outflows and the directions of measured proper motions of HH optical objects. We find that 6 out of 7 molecular outflows reported in OMC1-S (detection rate of 86%) have an extincted X-ray COUP star located at the expected position of the driving source. In several cases, X-rays detected the possible driving sources for the first time. This clustered embedded population revealed by Chandra is very young, with an estimated average age of few 10 5 yr. It is also likely responsible for the multiple HH objects, which are the optical correspondence of flows arising from the cloud. We show that the molecular outflows driven by the members of the OMC1-S cluster can account for the observed turbulence at core-scales and regulate the star formation efficiency. We discuss the effects of outflow feedback in the formation of massive stars, concluding that the injected turbulence in OMC1-S is compatible with a competitive accretion scenario.

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“…Two well-collimated bipolar CO outflows (outflows N and S) toward the northern part of the globule are reported in Beltrán et al (2012). In both outflows the blueshifted and redshifted lobes emanate from sources traced by their dust continuum emission (source C for outflow N and source I for outflow S), located at their symmetry center (see Fig.…”

Section: Introductionmentioning

confidence: 96%

“…Jets and outflows are ubiquitous in star-forming regions, but the cases of interaction between outflows are extremely rare. In fact, only two cases of apparent collision between jets or outflows are known, the IC 1396N outflows (Beltrán et al 2012) and BHR 71 (Zapata et al 2018). In BHR 71, the red lobe and the blue lobe of two different CO outflows collide, and in the area of interaction there is an increase of CO emission, and broadening of the lines, consistent with the collision scenario.…”

Section: Introductionmentioning

confidence: 99%

Collision of protostellar jets in the star-forming region IC 1396N. Analysis of knot proper motions

López,

Estalella,

Beltrán

et al. 2022

Preprint

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Context. The bright-rimmed cloud IC 1396N is believed to host one of the few known cases where two bipolar CO outflows driven by young stellar objects actually collide. The CO outflows are traced by chains of knots of H 2 emission, with enhanced emission at the position of the possible collision. Aims. The aim of this work is to use the proper motions of the H 2 knots to confirm the collision scenario. Methods. A second epoch H 2 image was obtained, and the proper motions of the knots were determined with a time baseline of ∼ 11 years. We also performed differential photometry on the images to check the flux variability of the knots. Results. For each outflow (N and S) we classified the knots as pre-collision or post-collision. The axes of the pre-collision knots, the position of the possible collision point, and the axes of the post-collision knots were estimated. The difference between the proper motion direction of the post-collision knots and the position angle from the collision point was also calculated. For some of the knots we obtained the 3D velocity by using the radial velocity derived from H 2 spectra. Conclusions. The velocity pattern of the H 2 knots in the area of interaction (post-collision knots) shows a deviation from that of the pre-collision knots, consistent with being a consequence of the interaction between the two outflows. This favours the interpretation of the IC 1396N outflows as a true collision between two protostellar jets instead of a projection effect.

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Close encounters of the protostellar kind in IC 1396N

Cited by 10 publications

References 16 publications

Properties of dense cores in clustered massive star-forming regions at high angular resolution

Properties of dense cores in clustered massive star-forming regions at high angular resolution

X-ray embedded stars as driving sources of outflow-driven turbulence in OMC1-S

Collision of protostellar jets in the star-forming region IC 1396N. Analysis of knot proper motions

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