The formation and destruction of molecular clouds and galactic star formation

Inutsuka, Shu‐ichiro; Inoue, Tsuyoshi; Iwasaki, Kazunari; Hosokawa, Takashi

doi:10.1051/0004-6361/201425584

Cited by 215 publications

(246 citation statements)

References 65 publications

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“…This then gives rise to a bimodal distribution of filamentary structures as observed in Musca. Recent numerical MHD simulations of molecular cloud formation tend to reproduce this pattern (Chen & Ostriker 2014;Inutsuka et al 2015, for example). The pattern observed in Musca is reminiscent of the situation seen around the Taurus B211/3 filament system, where velocity information is consistent with accretion of low-density striations onto the denser B211/3 filament (Goldsmith et al 2008;Palmeirim et al 2013).…”

Section: Magnetically-controlled Cloud and Filament Formationmentioning

confidence: 97%

“…First, large-scale compression of interstellar material due to, for example, an expanding bubble locally creates a finite-sized, self-gravitating layer with a magnetic field primarily in the plane of the dense layer of compressed gas (Inutsuka et al 2015, for example). Such a dense, self-gravitating layer is expected to fragment into one or several thermally supercritical filaments oriented perpendicular to the mean direction of the magnetic field (cf.…”

Section: Magnetically-controlled Cloud and Filament Formationmentioning

confidence: 99%

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Filamentary structure and magnetic field orientation in Musca

Cox

Arzoumanian

André

et al. 2016

A&A

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Herschel has shown that filamentary structures are ubiquitous in star-forming regions, in particular in nearby molecular clouds associated with Gould's Belt. High dynamic range far-infrared imaging of the Musca cloud with SPIRE and PACS reveals at least two types of filamentary structures: (1) the main ∼10-pc scale high column-density linear filament; and (2) low column-density striations in close proximity to the main filament. In addition, we find features with intermediate column densities (hair-like strands) that appear physically connected to the main filament. We present an analysis of this filamentary network traced by Herschel and explore its connection with the local magnetic field. We find that both the faint dust emission striations and the plane-of-the-sky (POS) magnetic field are locally oriented close to perpendicular to the high-density main filament (position angle ∼25−35 • ). The low-density striations and strands are oriented parallel to the POS magnetic field lines, which are derived previously from optical polarization measurements of background stars and more recently from Planck observations of dust polarized emission. The position angles are 97 ± 25 • , 105 ± 7 • , and 105 ± 5 • . From these observations, we propose a scenario in which local interstellar material in this cloud has condensed into a gravitationally-unstable filament (with "supercritical" mass per unit length) that is accreting background matter along field lines through the striations. We also compare the filamentary structure in Musca with what is seen in similar Herschel observations of the Taurus B211/3 filament system and find that there is significantly less substructure in the Musca main filament than in the B211/3 filament. We suggest that the Musca cloud may represent an earlier evolutionary stage in which the main filament has not yet accreted sufficient mass and energy to develop a multiple system of intertwined filamentary components.

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Section: Magnetically-controlled Cloud and Filament Formationmentioning

confidence: 97%

Section: Magnetically-controlled Cloud and Filament Formationmentioning

confidence: 99%

Filamentary structure and magnetic field orientation in Musca

Cox

Arzoumanian

André

et al. 2016

A&A

126

187

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“…We calculate the column density of CS molecules N CS in LTE using standard approach described by Mangum, Shirley (2015), Eq.80. In the beginning N CS is calculated under assumption that CS (2-1) line is optically thin but then optical depth correction factor, Goldsmith, Langer (1999), is used to make the value of N CS reliable. For diatomic linear molecules:…”

Section: Spatial Distribution Of the Molecular Gasmentioning

confidence: 99%

“…Theoretical calculations, e.g. Inutsuka et al (2015), predict formation of filamentary molecular clouds after multiple compression of interstellar gas by supersonic waves. So the periphery of extended bubbles (H regions or supernova remnants) could be reliable places for the formation of the molecular filaments.…”

Section: Introductionmentioning

confidence: 99%

“…So the filamentary structure could be an interesting example to test theoretical models by e.g. Inutsuka et al (2015). The aim of our study is to look for a dense gas in the inter-clump medium of the filamentary structure and check if it is a real physically connected structure or the clumps are separated from each other but embedded into a common gas envelope.…”

Section: Introductionmentioning

confidence: 99%

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Molecular gas in high-mass filament WB673

et al. 2017

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Abstract:We studied the distribution of dense gas in a filamentary molecular cloud containing several dense clumps. The center of the filament is given by the dense clump WB 673. The clumps are high-mass and intermediate-mass starforming regions. We observed CS (2-1), 13 CO (1-0), C 18 O (1-0), and methanol lines at 96 GHz toward WB 673 with the Onsala Space Observatory 20-m telescope. We found CS (2-1) emission in the inter-clump medium so the clumps are physically connected and the whole cloud is indeed a filament. Its total mass is 10 4 M ⊙ and mass-to-length ratio is 360 M ⊙ pc −1 from 13 CO (1-0) data. Mass-to-length ratio for the dense gas is 3.4 − 34 M ⊙ pc −1 from CS (2-1) data. The PV-diagram of the filament is V-shaped. We estimated physical conditions in the molecular gas using methanol lines. Location of the filament on the sky between extended shells suggests that it could be a good example to test theoretical models of formation of the filaments via multiple compression of interstellar gas by supersonic waves.

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The Molecular Cloud Lifecycle

et al. 2020

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Giant molecular clouds (GMCs) and their stellar offspring are the building blocks of galaxies. The physical characteristics of GMCs and their evolution are tightly connected to galaxy evolution. The macroscopic properties of the interstellar medium propagate into the properties of GMCs condensing out of it, with correlations between e.g. the galactic and GMC scale gas pressures, surface densities and volume densities. That way, the galactic environment sets the initial conditions for star formation within GMCs. After the onset of massive star formation, stellar feedback from e.g. photoionisation, stellar winds, and supernovae eventually contributes to dispersing the parent cloud, depositing energy, momentum and metals into the surrounding medium, thereby changing the properties of galaxies. This cycling of matter between gas and stars, governed by star formation and feedback, is therefore a major driver of galaxy evolution. Much of the recent debate has focused on the durations of the various evolutionary phases that constitute this cycle in galaxies, and what these can teach us about the physical mechanisms driving the cycle. We review results from observational, theoretical, and numerical work to build a dynamical picture of the evolutionary lifecycle of GMC evolution, star formation, and feedback in galaxies.

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The formation and destruction of molecular clouds and galactic star formation

Cited by 215 publications

References 65 publications

Filamentary structure and magnetic field orientation in Musca

Filamentary structure and magnetic field orientation in Musca

Molecular gas in high-mass filament WB673

The Molecular Cloud Lifecycle

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