2016MNRAS.461.2953H


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.14CEST14:09:46

2016MNRAS.461.2953H - Mon. Not. R. Astron. Soc., 461, 2953-2974 (2016/September-3)

Simulating radiative feedback and star cluster formation in GMCs - I. Dependence on gravitational boundedness.

HOWARD C.S., PUDRITZ R.E. and HARRIS W.E.

Abstract (from CDS):

Radiative feedback is an important consequence of cluster formation in giant molecular clouds (GMCs) in which newly formed clusters heat and ionize their surrounding gas. The process of cluster formation, and the role of radiative feedback, has not been fully explored in different GMC environments. We present a suite of simulations which explore how the initial gravitational boundedness, and radiative feedback, affect cluster formation. We model the early evolution (<5 Myr) of turbulent, 106 M clouds with virial parameters ranging from 0.5 to 5. To model cluster formation, we use cluster sink particles, coupled to a raytracing scheme, and a custom subgrid model which populates a cluster via sampling an initial mass function (IMF) with an efficiency of 20 per cent per free-fall time. We find that radiative feedback only decreases the cluster particle formation efficiency by a few per cent. The initial virial parameter plays a much stronger role in limiting cluster formation, with a spread of cluster formation efficiencies of 37-71 per cent for the most unbound to the most bound model. The total number of clusters increases while the maximum mass cluster decreases with an increasing initial virial parameter, resulting in steeper mass distributions. The star formation rates in our cluster particles are initially consistent with observations but rise to higher values at late times. This suggests that radiative feedback alone is not responsible for dispersing a GMC over the first 5 Myr of cluster formation.

Abstract Copyright: © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): hydrodynamics - radiative transfer - methods: numerical - stars: formation - ISM: clouds - H - regions - regions

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1131 0
2 NAME California Molecular Cloud MoC 04 10.0 +39 00           ~ 108 1
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3679 0
4 NAME Ori Complex Cld 05 35.3 -05 23           ~ 359 0
5 NAME Lup Cloud SFR 16 03 -38.1           ~ 558 0
6 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3156 1
7 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 351 1
8 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1514 0
9 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 460 0
10 NAME CrA Dark Cloud MoC 19 01 51 -36 58.9           ~ 412 0
11 NGC 7538 OpC 23 13 37 +61 30.0           ~ 834 0

    Equat.    Gal    SGal    Ecl

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2021.04.14-14:09:46

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