Classification of Filament Formation Mechanisms in Magnetized Molecular Clouds

Abe, Daisei; Inoue, Tsuyoshi; Inutsuka, Shu‐ichiro; Matsumoto, Toshiro

doi:10.3847/1538-4357/ac07a1

Cited by 38 publications

(31 citation statements)

References 63 publications

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“…Moreover, studies of Doi et al (2021) and Bialy et al (2021) have suggested that bubbles in the Perseus-Taurus region have formed the Perseus molecular cloud. Formation of clouds through expanding bubbles can result in an arc-shaped magnetic field morphology associated with the filamentary structures (Inoue & Fukui 2013;Inutsuka et al 2015;Inoue et al 2018;Abe et al 2021). These cloud-formation studies suggest that dense filamentary molecular clouds form via interaction of a shock front and a pre-existing inhomogeneous dense cloud, where the magnetic fields are predicted to bend and allow for further mass accumulation, creating even denser filaments.…”

Section: Introductionmentioning

confidence: 99%

3D magnetic-field morphology of the Perseus molecular cloud

Tahani

Lupypciw

Glover

et al. 2022

A&A

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Context. Despite recent observational and theoretical advances in mapping the magnetic fields associated with molecular clouds, their three-dimensional (3D) morphology remains unresolved. Multi-wavelength and multi-scale observations will allow us to paint a comprehensive picture of the magnetic fields of these star-forming regions. Aims. We reconstructed the 3D magnetic field morphology associated with the Perseus molecular cloud and compared it with predictions of cloud-formation models. These cloud-formation models predict a bending of magnetic fields associated with filamentary molecular clouds. We compared the orientation and direction of this field bending with our 3D magnetic-field view of the Perseus cloud. Methods. We used previous line-of-sight and plane-of-sky magnetic field observations as well as Galactic magnetic field models to reconstruct the complete 3D magnetic field vectors and morphology associated with the Perseus cloud. Results. We approximated the 3D magnetic field morphology of the cloud as a concave arc that points in the decreasing longitude direction in the plane of the sky (from our point of view). This field morphology preserves a memory of the Galactic magnetic field. In order to compare this morphology to cloud-formation model predictions, we assume that the cloud retains a memory of its most recent interaction. After incorporating velocity observations, we find that the line-of-sight magnetic field observations are consistent with predictions of shock-cloud-interaction models. Conclusions. To our knowledge, this is the first time that the 3D magnetic fields of a molecular cloud have been reconstructed. We find the 3D magnetic field morphology of the Perseus cloud to be consistent with the predictions of the shock-cloud-interaction model that describes the formation mechanism of filamentary molecular clouds.

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Section: Introductionmentioning

confidence: 99%

3D magnetic-field morphology of the Perseus molecular cloud

Tahani

Lupypciw

Glover

et al. 2022

A&A

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“…This velocity structure has also been observed toward another filament, the Musca filament (Bonne et al 2020). More recently, in a theoretical study, Abe et al (2021) proposed a classification of filament formation mechanisms resulting from the variation in the relative importance between the shock velocity, the turbulence, and the magnetic field strength (see also the theoretical study by Chen et al 2020a).…”

Section: Introductionmentioning

confidence: 99%

Velocity structure of the 50 pc long NGC 6334 filamentary cloud

Arzoumanian

Russeil

Zavagno

et al. 2022

A&A

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Context. The interstellar medium is observed to be organized in filamentary structures, and in neutral (H I) and ionized (H II) bubbles. The expanding nature of these bubbles shapes the surrounding medium and possibly plays a role in the formation and evolution of the interstellar filaments. The impact of the expansion of these bubbles on the interstellar medium is not well understood. Aims. Our aim is to describe the kinematics of a filamentary molecular cloud forming high-mass stars and hosting multiple H II regions in order to study the possible environmental impact on the properties of molecular filaments. Methods. We present APEX 13CO and C18O(2–1) mapping observations of the 10 × 50 pc NGC 6334 molecular cloud complex. We investigated the gas velocity structure along and across the 50 pc long cloud and toward velocity-coherent filaments (VCFs). Results. The NGC 6334 complex is observed to have a coherent velocity structure smoothly varying by ~5 km s−1 over its 50 pc elongation parallel to the Galactic plane. We identify a sample of 75 VCFs in the C18O(2–1) position-position-velocity cube and present the properties of 47 VCFs with a length ≳1 pc (five beams). We measure a large number of velocity gradients along the VCFs. The amplitudes of these velocity gradients and the velocity dispersion measured along the crests increase with the column density of the VCFs. We derive the column density and velocity power spectra of the VCFs. These power spectra are well represented with power laws showing similar slopes for the two quantities (with a mean of about −2), although some differ by up to a factor of 2. The position velocity diagrams perpendicular to three VCFs (selected from different physical environments) show the V-shaped velocity pattern corresponding to a bent structure in velocity space with the filament at the tip of the V surrounded by an extended structure connected to it with a velocity gradient. This velocity structure is qualitatively similar to that resulting from numerical simulations of filament formation from large-scale compression from propagating shock fronts. In addition, the radial profiles perpendicular to these VCFs hint to small-scale internal impacts from neighboring H II bubbles on two of them, while the third is mostly unaffected. Conclusions. The observed opposite curvature in velocity space (V- and A-shaped) toward the VCFs points to various origins of large-scale external compressions from propagating H I bubbles. This suggests the plausible importance of multiple H I compressions, separated in space and time, in the formation and evolution of molecular clouds and their star formation history. These atomic compressions due to past and distant star formation events are complemented by the impact of H II bubbles from present time and local star formation activity.

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“…Numerical simulations by Maeda et al (2021) demonstrated ∼10 4 M e massive clump formation driven by a large-scale H I gas flow that mimics galactic interactions. Abe et al (2021) showed that fast (>10 km s −1 ) gas flow is more favorable for massive filament formation with a line mass of >100 M e pc −1 . From observational perspectives, recent ALMA studies in M33 also found massive filaments with high-mass cluster formation associated with galaxy-galaxy interactions and other galaxyscale gas motions related to a spiral arm (Tokuda et al 2020;…”

Section: Colliding Flows Promoting the Protocluster Formation In N159...mentioning

confidence: 99%

An ALMA Study of the Massive Molecular Clump N159W-North in the Large Magellanic Cloud: A Possible Gas Flow Penetrating One of the Most Massive Protocluster Systems in the Local Group

Tokuda

Minami²,

Fukui

et al. 2022

ApJ

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Massive dense clumps in the Large Magellanic Cloud can be an important laboratory to explore the formation of populous clusters. We report multiscale ALMA observations of the N159W-North clump, which is the most CO-intense region in the galaxy. High-resolution CO isotope and 1.3 mm continuum observations with an angular resolution of ∼0.″25 (∼0.07 pc) revealed more than five protostellar sources with CO outflows within the main ridge clump. One of the thermal continuum sources, MMS-2, shows an especially massive/dense nature whose total H2 mass and peak column density are ∼104 M ⊙ and ∼1024 cm−2, respectively, and harbors massive (∼100 M ⊙) starless core candidates identified as its internal substructures. The main ridge containing this source can be categorized as one of the most massive protocluster systems in the Local Group. The CO high-resolution observations found several distinct filamentary clouds extending southward from the star-forming spots. The CO (1–0) data set with a larger field of view reveals a conical, ∼30 pc long complex extending toward the northern direction. These features indicate that a large-scale gas compression event may have produced the massive star-forming complex. Based on the striking similarity between the N159W-North complex and the other two previously reported high-mass star-forming clouds in the nearby regions, we propose a “teardrops inflow model” that explains the synchronized, extreme star formation across >50 pc, including one of the most massive protocluster clumps in the Local Group.

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Classification of Filament Formation Mechanisms in Magnetized Molecular Clouds

Cited by 38 publications

References 63 publications

3D magnetic-field morphology of the Perseus molecular cloud

3D magnetic-field morphology of the Perseus molecular cloud

Velocity structure of the 50 pc long NGC 6334 filamentary cloud

An ALMA Study of the Massive Molecular Clump N159W-North in the Large Magellanic Cloud: A Possible Gas Flow Penetrating One of the Most Massive Protocluster Systems in the Local Group

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