FILAMENTARY STRUCTURE OF STAR-FORMING COMPLEXES

By P. Myers. 2009

263 citations recorded by the source corpus.

The nearest young stellar groups are associated with “hubs” of column density exceeding 1022 cm−2, according to recent observations. These hubs radiate multiple “filaments” of parsec length, having lower column density and fewer stars. Systems with many filaments tend to have parallel filaments with similar spacing. Such “hub–filament structure” is associated with all of the nine young stellar groups within 300 pc, forming low-mass stars. Similar properties are seen in infrared dark clouds forming more massive stars. In a new model, an initial clump in a uniform medium is compressed into a self-gravitating, modulated layer. The outer layer resembles the modulated equilibrium of Schmid-Burgk with nearly parallel filaments. The filaments converge onto the compressed clump, which collapses to form stars with high efficiency. The initial medium and condensations have densities similar to those in nearby star-forming clouds and clumps. The predicted structures resemble observed hub–filament systems in their size, shape, and column density, and in the appearance of their filaments. These results suggest that HFS associated with young stellar groups may arise from compression of clumpy gas in molecular clouds.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/3e1b59aca4d282558a24d18ad8abdde2eac5581f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Spectroscopy

Citations in the corpus

A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey (2015, background): “…clouds were already known to exhibit large-scale filamentary structures long before Herschel (e.g., Schneider & Elmegreen 1979; Hartmann 2002; Myers 2009), the Herschel observations from the HGBS (e.g., Men’shchikov et al. 2010; Miville-Deschênes et al. 2010) and other imaging surveys such…”
SDC13 infrared dark clouds: longitudinally collapsing filaments? (2013, background): “In fact, SDC13 as a whole has a more complex geometry and density structure than the ones of a single filament, more like a hub-filament system (Myers 2009).”
Hierarchical fragmentation and differential star formation in the Galactic ‘Snake’: infrared dark cloud G11.11−0.12 (2014, methodology): “This configuration resembles the filamentary system discussed by Myers (2009) and may arise from compression of an elongated clump embedded in a thin cloud sheet, as seen in IRDC G14.”
An ALMA study of the Orion Integral Filament: I. Evidence for narrow fibers in a massive cloud (2018, background): “Morphologically speaking, the ISF fibers are distributed in multiple hub-like associations (Myers 2009) in both OMC-1 and OMC-2 regions.”
Cores, filaments, and bundles: hierarchical core formation in the L1495/B213 Taurus region (2013, background): “(See also Schneider & Elmegreen 1979; Johnstone & Bally 1999; Hartmann 2002; Myers 2009 for previous work emphasizing the importance of filaments in core formation.)”
Global hierarchical collapse in molecular clouds. Towards a comprehensive scenario (2019, background): “…et al. 2014; Hajigholi et al. 2016; Wyrowski et al. 2016; Juárez et al. 2017; Rayner et al. 2017; Lu et al. 2018; Baug et al. 2018; Gong et al. 2018; Ryabukhina et al. 2018; Dutta et al. 2018; Chen et al. 2019) that feeds central “hubs”, the sites where the filaments converge (Myers 2009).”
Global collapse of molecular clouds as a formation mechanism for the most massive stars (2013, background): “1), reminiscent of hub-filament systems (Myers 2009) observed in a number of low-mass (André et al. 2010; Peretto et al. 2012) and high-mass (Schneider et al. 2012; Hennemann et al. 2012) star-forming regions.”
Turbulent molecular clouds (2012, methodology): “Recently, this solution has been used by Myers (2009b) to model the hub filament structures that are often observed around young stellar groups.”
THE “NESSIE” NEBULA: CLUSTER FORMATION IN A FILAMENTARY INFRARED DARK CLOUD (2009, background): “Indeed, filamentary clouds may play an important role in high-mass star formation because they allow for enhanced accretion rates onto cores (Banerjee & Pudritz 2008; Myers 2009).”
FILAMENTARY ACCRETION FLOWS IN THE EMBEDDED SERPENS SOUTH PROTOCLUSTER (2013, background): “Observationally, young embedded cluster-forming systems are often found to be associated with multiple filaments, in a hubspoke like geometry (e.g., Myers 2009a).”
A CORRELATION BETWEEN SURFACE DENSITIES OF YOUNG STELLAR OBJECTS AND GAS IN EIGHT NEARBY MOLECULAR CLOUDS (2011, methodology): “…natal cloud material is needed to understand the nature of the distributed component, constrain models of star formation in molecular clouds, and ascertain the underlying physics that determine the density and rate of star formation (e.g. Bate & Bonnell 2005; Krumholz & Tan 2007; Myers 2009a).”
Filament Identification through Mathematical Morphology (2015, background): “Several qualitative descriptions of the filamentary networks have been proposed including a pervasive hubfilament structure (Myers 2009), converging filamentary patterns (Peretto et al. 2012b), or parallel networks (Busquet et al. 2013).”
A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, methodology): “…millimeter interferometers, such as SMA, CARMA, PdBI, and ALMA allow us to peer into molecular cores of individual proto-stars refining our understanding of how the molecular cloud core mass function is transformed into the initial mass function of stars and sub–stellar objects (e.g. Myers 2009).”
Dense core formation by fragmentation of velocity-coherent filaments in L1517 (2011, methodology): “This two-step scenario of core formation has already been proposed by several authors based on different considerations, and it therefore seems to apply to more regions than just the one studied here (Schneider & Elmegreen 1979; Hartmann 2002; Myers 2009).”