2010ApJ...709..191M


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.27CEST07:32:12

2010ApJ...709..191M - Astrophys. J., 709, 191-209 (2010/January-3)

The disruption of giant molecular clouds by radiation pressure and the efficiency of star formation in galaxies.

MURRAY N., QUATAERT E. and THOMPSON T.A.

Abstract (from CDS):

Star formation is slow in the sense that the gas consumption time is much longer than the dynamical time. It is also inefficient; star formation in local galaxies takes place in giant molecular clouds (GMCs), but the fraction of a GMC converted to stars is very small, εGMC∼ 5%. In luminous starbursts, the GMC lifetime is shorter than the main-sequence lifetime of even the most massive stars, so that supernovae can play no role in GMC disruption. We investigate the disruption of GMCs across a wide range of galaxies from normal spirals to the densest starbursts; we take into account the effects of H II gas pressure, shocked stellar winds, protostellar jets, and radiation pressure produced by the absorption and scattering of starlight on dust grains. In the Milky Way, a combination of three mechanisms–jets, H II gas pressure, and radiation pressure–disrupts the clouds. In more rapidly star-forming galaxies such as "clump" galaxies at high-redshift, ultra-luminous infrared galaxies (ULIRGs), and submillimeter galaxies, radiation pressure dominates natal cloud disruption. We predict the presence of ∼10-20 clusters with masses ∼107 M in local ULIRGs such as Arp 220 and a similar number of clusters with M*∼ 108 M in high redshift clump galaxies; submillimeter galaxies will have even more massive clusters. We find that εGMC = πGΣGMCc/(2(L/M*)) for GMCs that are optically thin to far-infrared radiation, where ΣGMC is the GMC gas surface density. The efficiency in optically thick systems continues to increase with ΣGMC, but more slowly, reaching ∼35% in the most luminous starbursts. The disruption of bubbles by radiation pressure stirs the interstellar medium (ISM) to velocities of ∼10 km/s in normal galaxies and to ∼100 km/s in ULIRGs like Arp 220, consistent with observations. Thus, radiation pressure may play a dominant dynamical role in the ISM of star-forming galaxies.

Abstract Copyright:

Journal keyword(s): galaxies: formation - galaxies: general - galaxies: starburst - galaxies: star clusters: general - H II regions - ISM: bubbles - ISM: clouds - stars: formation

Status at CDS:  

Simbad objects: 13

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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 - 2020
#notes
1 Bol 236 GlC 00 45 08.9030838047 +40 50 28.781102351 18.210 18.200 17.380 16.970 16.240 ~ 33 0
2 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5118 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14744 1
4 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5310 6
5 NAME Car Arm PoG 10 00 -60.0           ~ 376 1
6 [GS70] 298.2-00.3 HII 12 10 01.886 -62 50 00.46           ~ 65 1
7 [GCB88] 26 MoC 12 15.2 -62 47           ~ 6 0
8 GAL 298.9-00.4 HII 12 15 25.6 -63 01 28           ~ 15 0
9 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3762 4
10 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2668 4
11 W 49 SFR 19 10 20 +09 07.7           ~ 507 1
12 [ESS2003] Q2346-BX482 G 23 48 12.97 +00 25 46.3           ~ 34 0
13 [GCB88] 11 MoC ~ ~           ~ 2 0

    Equat.    Gal    SGal    Ecl

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2020.05.27-07:32:12

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