Massive stars in massive clusters – IV. Disruption of clouds by momentum-driven winds

Dale, James E.; Ngoumou, J.; Ercolano, Barbara; Bonnell, Ian A.

doi:10.1093/mnras/stt1822

Cited by 82 publications

(97 citation statements)

References 59 publications

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“…This limits the ability of SPH to capture the low but continuous mass-loss rate from massive stars, unless the mass resolution is very much better than in our whole galaxy simulations (see e.g. Dale et al 2013). In other words, it is much more difficult to obtain a resolved and converged evolution of stellar winds using SPH as opposed to in an Eulerian grid-based code that in principle has infinite mass resolution (albeit coupled with finite spatial resolution).…”

Section: Stellar Windsmentioning

confidence: 91%

Variable interstellar radiation fields in simulated dwarf galaxies: supernovae versus photoelectric heating

Naab

Glover

et al. 2017

Monthly Notices of the Royal Astronomical Society

127

222

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We present high-resolution hydrodynamical simulations of isolated dwarf galaxies including self-gravity, non-equilibrium cooling and chemistry, interstellar radiation fields (IRSF) and shielding, star formation, and stellar feedback. This includes spatially and temporally varying photoelectric (PE) heating, photoionization, resolved supernova (SN) blast waves and metal enrichment. A new flexible method to sample the stellar initial mass function allows us to follow the contribution to the ISRF, the metal output and the SN delay times of individual massive stars. We find that SNe play the dominant role in regulating the global star formation rate, shaping the multi-phase interstellar medium (ISM) and driving galactic outflows. Outflow rates (with massloading factors of a few) and hot gas fractions of the ISM increase with the number of SNe exploding in low-density environments where radiative energy losses are low. While PE heating alone can suppress star formation slightly more (a factor of a few) than SNe alone can do, it is unable to drive outflows and reproduce the multi-phase ISM that emerges naturally when SNe are included. These results are in conflict with recent results of Forbes et al. who concluded that PE heating is the dominant process suppressing star formation in dwarfs, about an order of magnitude more efficient than SNe. Potential origins for this discrepancy are discussed. In the absence of SNe and photoionization (mechanisms to disperse dense clouds), the impact of PE heating is highly overestimated owing to the (unrealistic) proximity of dense gas to the radiation sources. This leads to a substantial boost of the infrared continuum emission from the UV-irradiated dust and a far infrared line-to-continuum ratio too low compared to observations. Though sub-dominant in regulating star formation, the ISRF controls the abundance of molecular hydrogen via photodissociation.

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Section: Stellar Windsmentioning

confidence: 91%

Variable interstellar radiation fields in simulated dwarf galaxies: supernovae versus photoelectric heating

Naab

Glover

et al. 2017

Monthly Notices of the Royal Astronomical Society

127

222

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“…Dale et al (2012Dale et al ( , 2013 did extensive three-dimensional simulations of star cluster formation with ionization or stellar wind feedback and showed that the effects of photoionization and stellar winds are limited in quenching the star formation in massive molecular clouds (see also Walch et al 2012). Diaz-Miller et al (1998) calculated the steady-state structures of HII regions and pointed out that the photodissociation of hydrogen molecules due to far-ultraviolet (FUV) photons is much more important than photoionization due to UV photons for the destruction of molecular clouds.…”

Section: Quenching Of Star Formation In Molecular Cloudsmentioning

confidence: 99%

The formation and destruction of molecular clouds and galactic star formation

Inutsuka

Inoue

Iwasaki

et al. 2015

A&A

222

216

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We describe an overall picture of galactic-scale star formation. Recent high-resolution magneto-hydrodynamical simulations of twofluid dynamics with cooling, heating, and thermal conduction have shown that the formation of molecular clouds requires multiple episodes of supersonic compression. This finding enables us to create a scenario in which molecular clouds form in interacting shells or bubbles on a galactic scale. First, we estimated the ensemble-averaged growth rate of molecular clouds on a timescale longer than a million years. Next, we performed radiation hydrodynamics simulations to evaluate the destruction rate of magnetized molecular clouds by the stellar far-ultraviolet radiation. We also investigated the resulting star formation efficiency within a cloud, which amounts to a low value (a few percent) if we adopt the power-law exponent ∼− 2.5 for the mass distribution of stars in the cloud. We finally describe the time evolution of the mass function of molecular clouds on a long timescale (>1 Myr) and discuss the steady state exponent of the power-law slope in various environments.

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“…To have a fully physical description of a realistic selfregulation of star mass accretion and cluster formation, stellar feedbacks such as radiations (Bate 2009(Bate , 2012Price & Bate 2009;Commerçon et al 2011;Krumholz et al 2012), protostellar jets and outflows (Wang et al 2010;Nakamura & Li 2011Dale et al 2013cDale et al , 2015Federrath et al 2014;Federrath 2015), HII regions (Krumholz et al 2007;Peters et al 2010;Dale et al 2013aDale et al ,b, 2015Geen et al 2015), and supernovae (Iffrig & Hennebelle 2015;Walch & Naab 2015) should be incorporated. We limit ourselves to the simple scenario without feedback mechanisms, in which nothing except the depletion of cloud gas can stop sink accretion.…”

Section: Qualitative Presentationsmentioning

confidence: 99%

Formation of a protocluster: A virialized structure from gravoturbulent collapse

Lee

Hennebelle

2016

A&A

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Context. Stars are often observed to form in clusters and it is therefore important to understand how such a region of concentrated mass is assembled out of the diffuse medium. The properties of such a region eventually prescribe the important physical mechanisms and determine the characteristics of the stellar cluster. Aims. We study the formation of a gaseous protocluster inside a molecular cloud and associate its internal properties with those of the parent cloud by varying the level of the initial turbulence of the cloud with a view to better characterize the subsequent stellar cluster formation. Methods. We performed high resolution magnetohydrodynamic (MHD) simulations of gaseous protoclusters forming in molecular clouds collapsing under self-gravity. We determined ellipsoidal cluster regions via gas kinematics and sink particle distribution, permitting us to determine the mass, size, and aspect ratio of the cluster. We studied the cluster properties, such as kinetic and gravitational energy, and made links to the parent cloud. Results. The gaseous protocluster is formed out of global collapse of a molecular cloud and has non-negligible rotation owing to angular momentum conservation during the collapse of the object. Most of the star formation occurs in this region, which occupies only a small volume fraction of the whole cloud. This dense entity is a result of the interplay between turbulence and gravity. We identify such regions in simulations and compare the gas and sink particles to observed star-forming clumps and embedded clusters, respectively. The gaseous protocluster inferred from simulation results presents a mass-size relation that is compatible with observations. We stress that the stellar cluster radius, although clearly correlated with the gas cluster radius, depends sensitively on its definition. Energy analysis is performed to confirm that the gaseous protocluster is a product of gravoturbulent reprocessing and that the support of turbulent and rotational energy against self-gravity yields a state of global virial equilibrium, although collapse is occurring at a smaller scale and the cluster is actively forming stars. This object then serves as the antecedent of the stellar cluster, to which the energy properties are passed on. Conclusions. The gaseous protocluster properties are determined by the parent cloud out of which it forms, while the gas is indeed reprocessed and constitutes a star-forming environment that is different from that of the parent cloud.

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Massive stars in massive clusters – IV. Disruption of clouds by momentum-driven winds

Cited by 82 publications

References 59 publications

Variable interstellar radiation fields in simulated dwarf galaxies: supernovae versus photoelectric heating

Variable interstellar radiation fields in simulated dwarf galaxies: supernovae versus photoelectric heating

The formation and destruction of molecular clouds and galactic star formation

Formation of a protocluster: A virialized structure from gravoturbulent collapse

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