Massive Star Formation

Tan, Jonathan C.; Beltrán, M. T.; Caselli, P.; Fontani, F.; Fuente, A.; Krumholz, Mark R.; McKee, Christopher F.; Stolte, A.

doi:10.2458/azu_uapress_9780816531240-ch007

Cited by 210 publications

(224 citation statements)

References 4 publications

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“…Because gravitational collapse will start for those clumps for which the free-fall time is less than the dynamical time, this result suggests that clumps with higher masses are more susceptible to gravitational instabilities and they evolve faster than their lower mass counterparts (see Figure 3). This is in agreement with the theoretical picture for high-mass star formation, where clumps with higher mass evolve faster, quickly disrupting their natal environment (e.g., Tan et al 2014).…”

Section: Free-fall Time and Dynamical Time Of The Clumpssupporting

confidence: 80%

Characterizing the properties of cluster precursors in the MALT90 survey

Contreras

Rathborne

Guzmán

et al. 2016

Mon. Not. R. Astron. Soc.

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In the Milky Way there are thousands of stellar clusters each harboring from a hundred to a million stars. Although clusters are common, the initial conditions of cluster formation are still not well understood. To determine the processes involved in the formation and evolution of clusters it is key to determine the global properties of cluster-forming clumps in their earliest stages of evolution. Here, we present the physical properties of 1,244 clumps identified from the MALT90 survey. Using the dust temperature of the clumps as a proxy for evolution we determined how the clump properties change at different evolutionary stages. We find that less-evolved clumps exhibiting dust temperatures lower than 20 K have higher densities and are more gravitationally bound than more-evolved clumps with higher dust temperatures. We also identified a sample of clumps in a very early stage of evolution, thus potential candidates for high-mass star-forming clumps. Only one clump in our sample has physical properties consistent with a young massive cluster progenitor, reinforcing the fact that massive proto-clusters are very rare in the Galaxy.

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Section: Free-fall Time and Dynamical Time Of The Clumpssupporting

confidence: 80%

Characterizing the properties of cluster precursors in the MALT90 survey

Contreras

Rathborne

Guzmán

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The evolution of an SF system is an integral part of the ISM ecology and it starts from molecular cloud formation and ends with the destruction of the cloud by radiation and winds of massive stars, supernova explosions, dispersion of open clusters of massive stars or massive globular cluster formation. Above we have briefly discussed some aspects of the first stages of the SF process and a more detailed discussion can be found in Bromm and Larson (2004), McKee and Ostriker (2007), Zinnecker and Yorke (2007), Elmegreen (2011a), Kennicutt and Evans (2012), Sanchez Almeida et al (2014), Krumholz (2014), Molinari et al (2014), and Tan et al (2014).…”

Section: Hydrodynamical Models Of Massive Star Winds and Superbubblesmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

111

102

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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“…3, c.f. Tan et al 2014) corresponding to a high concentration of mass. Eighty percent of the clumps host MDCs above 40 M and the most massive fragments scale with the mass of their clump.…”

Section: Limited Fragmentation From Clump To Core Scalementioning

confidence: 99%

ALMA survey of massive cluster progenitors from ATLASGAL

Csengeri

Bontemps²,

Wyrowski

et al. 2017

A&A

Self Cite

108

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The early evolution of massive cluster progenitors is poorly understood. We investigate the fragmentation properties from 0.3 pc to 0.06 pc scales of a homogenous sample of infrared-quiet massive clumps within 4.5 kpc selected from the ATLASGAL survey. Using the ALMA 7 m array we detect compact dust continuum emission towards all targets and find that fragmentation, at these scales, is limited. The mass distribution of the fragments uncovers a large fraction of cores above 40 M , corresponding to massive dense cores (MDCs) with masses up to ∼400 M . Seventyseven percent of the clumps contain at most 3 MDCs per clump, and we also reveal single clumps/MDCs. The most massive cores are formed within the more massive clumps and a high concentration of mass on small scales reveals a high core formation efficiency. The mass of MDCs highly exceeds the local thermal Jeans mass, and we lack the observational evidence of a sufficiently high level of turbulence or strong enough magnetic fields to keep the most massive MDCs in equilibrium. If already collapsing, the observed fragmentation properties with a high core formation efficiency are consistent with the collapse setting in at parsec scales.

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Massive Star Formation

Cited by 210 publications

References 4 publications

Characterizing the properties of cluster precursors in the MALT90 survey

Characterizing the properties of cluster precursors in the MALT90 survey

Nonthermal particles and photons in starburst regions and superbubbles

ALMA survey of massive cluster progenitors from ATLASGAL

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