scholarly journals Ambipolar Drift Heating in Turbulent Molecular Clouds

2000 ◽  
Vol 540 (1) ◽  
pp. 332-341 ◽  
Author(s):  
Paolo Padoan ◽  
Ellen Zweibel ◽  
Ake Nordlund
Keyword(s):  
Molecular Clouds ◽  
Ambipolar Drift

ERRATUM: “AMBIPOLAR DRIFT HEATING IN TURBULENT MOLECULAR CLOUDS” (2000, ApJ, 540, 332)

2012 ◽  
Vol 755 (2) ◽  
pp. 182 ◽  
Author(s):  
Paolo Padoan ◽  
Ellen Zweibel ◽  
Åke Nordlund
Keyword(s):  
Molecular Clouds ◽  
Ambipolar Drift

Structure of the turbulent atomic gas and formation of molecular clouds

2008 ◽  
Vol 31 ◽  
pp. 15-18
Author(s):  
P. Hennebelle ◽  
E. Audit
Keyword(s):  
Molecular Clouds ◽  
Atomic Gas

Transport of Dust Grains in Turbulent Molecular Clouds

1998 ◽  
Vol 498 (2) ◽  
pp. 757-762 ◽  
Author(s):  
B. R. Ragot
Keyword(s):  
Molecular Clouds ◽  
Dust Grains

scholarly journals Molecules in the Magellanic Clouds

1991 ◽  
Vol 148 ◽  
pp. 415-420 ◽  
Author(s):  
R. S. Booth ◽  
Th. De Graauw
Keyword(s):  
High Resolution ◽  
Molecular Clouds ◽  
Short Review ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Giant Molecular Clouds ◽  
Interstellar Molecules ◽  
First Time ◽  
Excitation Conditions

In this short review we describe recent new observations of millimetre transitions of molecules in selected regions of the Magellanic Clouds. The observations were made using the Swedish-ESO Submillimetre Telescope, SEST, (Booth et al. 1989), the relatively high resolution of which facilitates, for the first time, observations of individual giant molecular clouds in the Magellanic Clouds. We have mapped the distribution of the emission from the two lowest rotational transitions of 12CO and 13CO and hence have derived excitation conditions for the molecule. In addition, we have observed several well-known interstellar molecules in the same regions, thus doubling the number of known molecules in the Large Magellanic Cloud (LMC). The fact that all the observations have been made under controlled conditions with the same telescope enables a reasonable intercomparison of the molecular column densities. In particular, we are able to observe the relative abundances among the different isotopically substituted species of CO.

Compact cores of molecular clouds in NGC 1333/IRAS 6–9

2000 ◽  
Vol 24 (4) ◽  
pp. 511-521
Author(s):  
Jin Sun ◽  
Jia-jian Shen ◽  
Yan-ping Zhang ◽  
Jin-jiang Sun
Keyword(s):  
Molecular Clouds

scholarly journals Effects of initial density profiles on massive star cluster formation in giant molecular clouds

2021 ◽  
Author(s):  
Yingtian Chen ◽  
Hui Li ◽  
Mark Vogelsberger
Keyword(s):  
Angular Momentum ◽  
Star Formation ◽  
Molecular Clouds ◽  
Globular Clusters ◽  
Cluster Formation ◽  
Initial Density ◽  
Giant Molecular Clouds ◽  
Density Profiles ◽  
Stellar Feedback ◽  
Gas Accretion

Abstract We perform a suite of hydrodynamic simulations to investigate how initial density profiles of giant molecular clouds (GMCs) affect their subsequent evolution. We find that the star formation duration and integrated star formation efficiency of the whole clouds are not sensitive to the choice of different profiles but are mainly controlled by the interplay between gravitational collapse and stellar feedback. Despite this similarity, GMCs with different profiles show dramatically different modes of star formation. For shallower profiles, GMCs first fragment into many self-gravitation cores and form sub-clusters that distributed throughout the entire clouds. These sub-clusters are later assembled ‘hierarchically’ to central clusters. In contrast, for steeper profiles, a massive cluster is quickly formed at the center of the cloud and then gradually grows its mass via gas accretion. Consequently, central clusters that emerged from clouds with shallower profiles are less massive and show less rotation than those with the steeper profiles. This is because 1) a significant fraction of mass and angular momentum in shallower profiles is stored in the orbital motion of the sub-clusters that are not able to merge into the central clusters 2) frequent hierarchical mergers in the shallower profiles lead to further losses of mass and angular momentum via violent relaxation and tidal disruption. Encouragingly, the degree of cluster rotations in steeper profiles is consistent with recent observations of young and intermediate-age clusters. We speculate that rotating globular clusters are likely formed via an ‘accretion’ mode from centrally-concentrated clouds in the early Universe.

Sign in / Sign up

Export Citation Format

Share Document