2019A&A...629A..81T


Query : 2019A&A...629A..81T

2019A&A...629A..81T - Astronomy and Astrophysics, volume 629A, 81-81 (2019/9-1)

Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2.

TREVINO-MORALES S.P., FUENTE A., SANCHEZ-MONGE A., KAINULAINEN J., DIDELON P., SURI S., SCHNEIDER N., BALLESTEROS-PAREDES J., LEE Y.-N., HENNEBELLE P., PILLERI P., GONZALEZ-GARCIA M., KRAMER C., GARCIA-BURILLO S., LUNA A., GOICOECHEA J.R., TREMBLIN P. and GEEN S.

Abstract (from CDS):


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 13CO and C18O 1-0 and 2-1 lines obtained with the IRAM-30 m telescope. We also used H2 column density maps derived from Herschel dust emission observations.
Results. We identified the filamentary network in Mon R2 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 30-100M/pc and show signs of fragmentation, while the secondary filaments have line masses of 12-60M/pc 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 10–4-10–3M/yr into the central hub. The secondary filaments accrete into the main filaments at a rate of 0.1-0.4x10–4M/yr. 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 ∼2.5Myr, 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.

Abstract Copyright: © ESO 2019

Journal keyword(s): ISM: kinematics and dynamics - ISM: structure - ISM: clouds - ISM: individual objects: Monoceros R2

CDS comments: Filaments not in SIMBAD.

Simbad objects: 13

goto Full paper

goto View the references in ADS

Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1239 0
2 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 256 0
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4015 0
4 NAME Ori A MoC 05 38 -07.1           ~ 2870 0
5 NAME Mon R2 Cluster Cl* 06 07 45 -06 22.8           ~ 18 0
6 NAME Mon R2 IRS 4 * 06 07 45.25 -06 23 19.9           ~ 18 0
7 NAME Mon R2 IRS 5 * 06 07 45.6 -06 22 40           ~ 16 0
8 NAME Mon R2 IRS 2 * 06 07 45.83 -06 22 53.5           B0 107 0
9 NAME Mon R2 IRS 1 cor 06 07 46.20 -06 23 09.5           B0 62 0
10 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 702 2
11 NAME Mon R2 IRS 3 Y*O 06 07 47.8 -06 22 55           ~ 139 0
12 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1030 2
13 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 1010 0

To bookmark this query, right click on this link: simbad:objects in 2019A&A...629A..81T and select 'bookmark this link' or equivalent in the popup menu


2022.10.01-13:54:36

© Université de Strasbourg/CNRS

    • Contact