Filamentary Accretion Flows in the Embedded Serpens South Protocluster

Kirk, Helen; Myers, Philip C.; Bourke, Tyler L.; Gutermuth, Robert; Hedden, Abigail; Wilson, Grant

doi:10.1088/0004-637x/766/2/115

Cited by 308 publications

(435 citation statements)

References 56 publications

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“…We can also see many faint filamentary structures that mimic "striations" observed in the Taurus dark cloud and are almost parallel to the mean magnetic field lines (Goldsmith et al 2008). In our simulations, these faint filaments appear to be feeding gas onto dense filaments (similar to what is observed for local clouds by e.g., Sugitani et al 2011;Palmeirim et al 2013;Kirk et al 2013). Once the line mass of a dense filament exceeds the critical value (2C 2 s /G), star formation is expected to start (Inutsuka & Miyama 1992André et al 2010).…”

Section: Introductionsupporting

confidence: 84%

The formation and destruction of molecular clouds and galactic star formation

Inutsuka

Inoue

Iwasaki

et al. 2015

A&A

229

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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Section: Introductionsupporting

confidence: 84%

The formation and destruction of molecular clouds and galactic star formation

Inutsuka

Inoue

Iwasaki

et al. 2015

A&A

229

216

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“…For a filamentary inflow, the mass accretion rate can be described byṀ = πr 2 n(H 2 ) × V infall (R) (e.g., see Kirk et al 2013). Falling from a distance R = 0.8 pc (see Sect.…”

Section: Discussionmentioning

confidence: 99%

Gravitational collapse of the OMC-1 region

Hacar

Tafalla

Goicoechea

2017

A&A

104

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We have investigated the global dynamical state of the integral shaped filament in the Orion A cloud using new N 2 H + (1−0) largescale, IRAM 30 m observations. Our analysis of its internal gas dynamics reveals the presence of accelerated motions towards the Orion Nebula Cluster, showing a characteristic blue-shifted profile centred at the position of the OMC-1 South region. The properties of these observed gas motions (profile, extension, and magnitude) are consistent with the expected accelerations for the gravitational collapse of the OMC-1 region and explain both the physical and kinematic structure of this cloud.

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“…Rescaled to the same distance, the virial mass for the entire Aquila Rift estimated by Dame & Thaddeus (1985) is ∼3.3 × 10 5 M , suggesting that the whole complex is close to virial balance on large scales. More recently, Tanaka et al (2013) obtained a virial parameter ∼0.08-0.24 for the Serpens South filament (again rescaled to a distance of 260 pc) on ∼0.5 pc scales (see also Kirk et al 2013a), and Maury et al (2011) derived a high star formation rate of ∼23 M Myr −1 pc −2 for the protocluster associated with the filament (of total mass ∼610 M , also using d = 260 pc). Altogether, these results suggest that the Aquila Rift complex is globally gravitationally bound on scales of ∼25 pc and includes a few highly unstable (sub-virial) clumps on the verge of forming rich star clusters on sub-parsec scales.…”

Section: The Aquila Rift Regionmentioning

confidence: 99%

A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from theHerschelGould Belt survey

Könyves

André

Men’shchikov

et al. 2015

A&A

408

471

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We present and discuss the results of the Herschel Gould Belt survey (HGBS) observations in an ∼11 deg 2 area of the Aquila molecular cloud complex at d ∼ 260 pc, imaged with the SPIRE and PACS photometric cameras in parallel mode from 70 μm to 500 μm. Using the multi-scale, multi-wavelength source extraction algorithm getsources, we identify a complete sample of starless dense cores and embedded (Class 0-I) protostars in this region, and analyze their global properties and spatial distributions. We find a total of 651 starless cores, ∼60% ± 10% of which are gravitationally bound prestellar cores, and they will likely form stars in the future. We also detect 58 protostellar cores. The core mass function (CMF) derived for the large population of prestellar cores is very similar in shape to the stellar initial mass function (IMF), confirming earlier findings on a much stronger statistical basis and supporting the view that there is a close physical link between the stellar IMF and the prestellar CMF. The global shift in mass scale observed between the CMF and the IMF is consistent with a typical star formation efficiency of ∼40% at the level of an individual core. By comparing the numbers of starless cores in various density bins to the number of young stellar objects (YSOs), we estimate that the lifetime of prestellar cores is ∼1 Myr, which is typically ∼4 times longer than the core free-fall time, and that it decreases with average core density. We find a strong correlation between the spatial distribution of prestellar cores and the densest filaments observed in the Aquila complex. About 90% of the Herschel-identified prestellar cores are located above a background column density corresponding to A V ∼ 7, and ∼75% of them lie within filamentary structures with supercritical masses per unit length > ∼ 16 M /pc. These findings support a picture wherein the cores making up the peak of the CMF (and probably responsible for the base of the IMF) result primarily from the gravitational fragmentation of marginally supercritical filaments. Given that filaments appear to dominate the mass budget of dense gas at A V > 7, our findings also suggest that the physics of prestellar core formation within filaments is responsible for a characteristic "efficiency" SFR/M dense ∼ 5 +2 −2 × 10 −8 yr −1 for the star formation process in dense gas.

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Filamentary Accretion Flows in the Embedded Serpens South Protocluster

Cited by 308 publications

References 56 publications

The formation and destruction of molecular clouds and galactic star formation

The formation and destruction of molecular clouds and galactic star formation

Gravitational collapse of the OMC-1 region

A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from theHerschelGould Belt survey

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