Unbound clouds and the star formation efficiency 80
Molecular Clouds and Star Formation
... Membership in the Cepheus OB3 association and in its individual subgroups, the ages and kinematics of the stars, and the structure and energetics of the related [r] ...
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CiteSeerX — The Velocity Field and the Star Formation Efficiency in Molecular Clouds. I. The Non-Magnetic Case
... 2006; Whitworth et al. 2007; G´ omez et al. 2007), so that the mass of the structures must grow over time, possibly eventually becoming strongly self-gravitating and proceed- ing to collapse. However, even if these cores ...
10
CiteSeerX — Clumps and triggered star formation in ionised molecular clouds
... In the bottom panel of Fig. 10 we plot the mean mass accretion rates onto sinks up to t 15 , ˙ M, as a function of their masses, M 15 . Above and to the right of the dotted lines a sink that continues to accrete at the ...
12
The earliest fragmentation in molecular clouds : and its connection to star formation
... sitions of their clumps and their masses do not correspond with each other. As the density distribution of molecular clouds is hierarchical with structure on all scales it is unclear which scale is the most ...
171
Density, Alternative Determinant of Star Formation Efficiency of the Milky Way GMCs: Core Reason for Low Star Formation Efficiency
... overall efficiency with which Milky Way Giant Molecular Clouds (GMCs) is forming stars was determined by deriving an equation using density of cloud ...determines star formation other than the ...
The star formation history of the Magellanic Clouds derived from long-period variable star counts
... Magellanic Clouds – galaxies: star formation – galaxies: stellar content – galaxies: ...Magellanic Clouds (Large, LMC, and Small, SMC) are irregu- lar, gas-rich dwarf galaxies in our Local ...
9
The Location, Clustering, and Propagation of Massive Star Formation in Giant Molecular Clouds
... their formation pathway remains ...molecular clouds ( GMCs ) , and ∼ 100 young (< 10 Myr ) optical stellar clusters ( SCs ) in the Large Magellanic ...massive star formation and its relation ...
14
Molecular Clouds and Star Formation: A Multiwavelength Study of Perseus, Serpens, and Ophiuchus
... of star formation at Caltech can be a lonely ven- ture at times, but I have been lucky enough to have a number of collaborators at other institutions who have taken interest in my work, particularly Neal ...
332
Magnetic diffusion in star formation: From clouds to cores to stars to disks
... This problem, as the ones previously discussed, will be solved using high-resolution, long-term, physically-accurate and complete, self-consistent numerical simulations. This should ideally happen as part of a larger ...
203
The dynamical evolution of molecular clouds near the Galactic Centre -- III. Tidally--induced star formation in protocluster clouds
... isolated clouds first (dotted lines), the HDens and LVir simulations form stars at the highest ...a star–formation efficiency of ...(0.31) clouds. All three of these clouds have ...
22
Dynamical Masses of Young Star Clusters: Constraints on the Stellar IMF and Star-Formation Efficiency
... 1 University College London [email protected] 2 University of Sheffield [email protected] 1 The Stellar Initial Mass Function in Clusters Many recent works have attempted to constrain the stellar initial ...
5
Duration of Star Formation in Galactic Giant Molecular Clouds. I. The Great Nebula in Carina
... A number of systematics, in particular neglect of stel- lar accretion histories and treating binary systems as single stars, both of which we have done here, are known to contribute to apparent isochronal age spreads of ...
24
The W43 MM1 mini starburst ridge, a test for star formation efficiency models
... 2010). Their exact choice, at this stage, is dictated by the reason- able agreement with the data on the SFR. Before comparing our results with the models, we would like to stress that all models have similar behaviors. ...
10
Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies. João Alves, University of Vienna
... 4. The integrated SFR scales linearly with, and is most reliably traced by, the dense gas mass in a star forming region. 6. The Kennicutt-Schmidt law for galaxies is largely the result of unresolved measurements ...
88
From Large-scale Molecular Clouds to Filaments and Cores : Unveiling the Role of the Magnetic Fields in Star Formation
... 1.4. E vidence of magnetic field 9 of measuring the line-of-sight component of the field strength (Crutcher et al., 2010). It is the splitting of a spectral line into several components in the presence of a static ...
133
Star cluster evolution in the Magellanic Clouds revisited
... Goodwin & Bastian (2006), most dissolving clusters will have dispersed by an age of ∼ 30 Myr, while the surviving clusters will have returned to an equilibrium state by ∼ 40 Myr, when some of the early expansion will ...
7
Can the removal of molecular cloud envelopes by external feedback affect the efficiency of star formation?
... how star formation efficiency can be significantly decreased by the removal of a molecular cloud’s envelope by feedback from an external ...from star formation has difficulties halting ...
10
The Relationship Between Molecular Gas, H I, and Star Formation in the Low-mass, Low-metallicity Magellanic Clouds
... Magellanic Clouds provide the only laboratory to study the effects of metallicity and galaxy mass on molecular gas and star formation at high (∼ 20 pc ) ...Magellanic Clouds, avoiding the ...
24
Star formation in Galactic flows
... of the individual object, the larger scale region, or the compression time due to the large-scale spiral shock. 3 F L OW DY N A M I C S I N S I D E S P I R A L A R M The first goal is to establish where in the simulation ...
8
The quenching of star formation in galaxies
... 1.3.2 Star formation The details of cloud collapse and subsequent star formation are not well ...cooling clouds become cold and ...the star to persist in a quasi-static pressure ...
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