Perception of Interstellar Structure: Facing Complexity

Scalo, J. M.

doi:10.1007/978-94-009-0605-1_12

Cited by 130 publications

(22 citation statements)

References 70 publications

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“…Turbulence holds the key to many crucial galactic processes such as star formation [167,173], cloud structure and dynamics [234] and the evolution of the different phases of the ISM. Its characterization on Galactic scales is necessary to evaluate its impact on Galactic evolution (see models by Gazol-Patiño and Passot [108] and references therein).…”

Section: Turbulence In the Milky Waymentioning

confidence: 99%

Science with ASKAP

et al. 2008

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The future of cm and m-wave astronomy lies with the Square Kilometre Array (SKA), a telescope under development by a consortium of 17 countries. The SKA will be 50 times more sensitive than any existing radio facility. A majority of the key science for the SKA will be addressed through large-area imaging of the Universe at frequencies from 300 MHz to a few GHz. The Australian SKA Pathfinder (ASKAP) is aimed squarely in this frequency range, and achieves instantaneous wide-area imaging through the development and deployment of phase-array feed systems on parabolic reflectors. This large field-of-view makes ASKAP an unprecedented synoptic telescope poised J. Wall is the overall editor.

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Section: Turbulence In the Milky Waymentioning

confidence: 99%

Science with ASKAP

et al. 2008

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“…In particular, in those models, the time required for building up a giant MC (∼ 100 Myr) is so long that it is difficult to either support a GMC against collapse, or avoid their disruption by the internal HII regions and SN explosions. In addition to the fact that there is not enough molecular material in the "chaff" to allow the formation of GMCs via agglomeration (Blitz & Williams, 1999), the picture of "cloudlets" flying ballistically might be inadequate, since clouds are not a collection of isolated entities of gas, but an interconnected network that has only been made to look like spheres due to the limitations of the observations (Scalo, 1990).…”

Section: Cloud Formation and Destructionmentioning

confidence: 99%

Molecular Clouds: Formation and Disruption

Ballesteros-Paredes¹

2004

Astrophysics and Space Science

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Abstract.Molecular clouds (MC) are the densest and coldest component of the interstellar gas, and the sites of star formation. They are also turbulent and fractal and their masses and sizes span several orders of magnitude. It is also generally believed that they are close to Virial equilibrium (VE). Since this statement has been questioned by a number of authors, with important implications on molecular clouds' lifetimes, we will review this subject within the context of a turbulent ISM. In this framework, there is significant numerical evidence that MCs are not in VE, that there is a strong exchange of mass, momentum and energy between clouds and their surrounding medium, and that it is difficult (if not impossible) to form quasistatic cores inside MCs, suggesting that they must be transient, short-lived phenomena. Thus, their formation and disruption must be primarily dynamical, and probably not due to just a single mechanism, but rather to the combination of several processes. This picture seems consistent with recent estimates of ages of stars in the solar neighborhood.

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“…The most obvious application of this model is to the formation of clumps inside clouds (Sasao 1973;Scalo 1990;Falgarone and Phillips 1990;Porter, et al 1992;Yue et al 1993). Such a formation mechanism presumably accounts for the fractal appearance of the cloud boundaries and the hierarchy of scales inside the clouds.…”

Section: Cloud Formation By Compression In Supersonic Turbulencementioning

confidence: 99%