Dynamics of cluster-forming hub-filament systems The case of the high-mass star-forming complex Monoceros R2
Artikel i vetenskaplig tidskrift, 2019

Context. High-mass stars and star clusters commonly form within hub-filament systems. Monoceros R2 (hereafter Mon R2), at a distance of 830 pc, harbors one of the closest of these systems, making it an excellent target for case studies. Aims. We investigate the morphology, stability and dynamical properties of the Mon R2 hub-filament system. Methods. We employed observations of the (CO)-C-13 and (CO)-O-18 1 -> 0 and 2 -> 1 lines obtained with the IRAM-30m telescope. We also used H-2 column density maps derived from Herschel dust emission observations. Results. We identified the filamentary network in Mon R-2 with the DisPerSE algorithm and characterized the individual filaments as either main (converging into the hub) or secondary (converging to a main filament). The main filaments have line masses of 30-100 M-circle dot pc(-1) and show signs of fragmentation, while the secondary filaments have line masses of 12-60 M-circle dot pc(-1) and show fragmentation only sporadically. In the context of Ostriker's hydrostatic filament model, the main filaments are thermally supercritical. If non-thermal motions are included, most of them are transcritical. Most of the secondary filaments are roughly transcritical regardless of whether non-thermal motions are included or not. From the morphology and kinematics of the main filaments, we estimate a mass accretion rate of 10(-4)-10(-3) M-circle dot yr(-1) into the central hub. The secondary filaments accrete into the main filaments at a rate of 0.1-0.4 x 10(-4) M-circle dot yr(-1). The main filaments extend into the central hub. Their velocity gradients increase toward the hub, suggesting acceleration of the gas. We estimate that with the observed infall velocity, the mass-doubling time of the hub is similar to 2.5 Myr, ten times longer than the free-fall time, suggesting a dynamically old region. These timescales are comparable with the chemical age of the HII region. Inside the hub, the main filaments show a ring-or a spiral-like morphology that exhibits rotation and infall motions. One possible explanation for the morphology is that gas is falling into the central cluster following a spiral-like pattern.

ISM: kinematics and dynamics

ISM: clouds

ISM: individual objects: Monoceros R2

ISM: structure


Sandra Treviño Morales

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Galaktisk astrofysik

A. Fuente

Observatorio Astronómico Nacional (OAN)

A. Sanchez-Monge

Universität zu Köln

Jouni Kainulainen

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Galaktisk astrofysik

P. Didelon

Université Paris Diderot

S. Suri


Universität zu Köln

N. Schneider

Universität zu Köln

J. Ballesteros-Paredes

Universidad Nacional Autonoma de Mexico

Y. -N. Lee

Université Paris Diderot

P. Hennebelle

Université Paris Diderot

P. Pilleri

Université de Toulouse

M. Gonzalez-Garcia

Consejo Superior de Investigaciones Científicas (CSIC)

C. Kramer

Institut de RadioAstronomie Millimetrique (IRAM)

S. Garcia-Burillo

Observatorio Astronómico Nacional (OAN)

A. Luna

Instituto Nacional de Astrofísica, Óptica y Electrońica

J. R. Goicoechea

Consejo Superior de Investigaciones Científicas (CSIC)

P. Tremblin

Université Paris Diderot

S. Geen

Universität Heidelberg

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 629 A81


Astronomi, astrofysik och kosmologi





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