Pith. sign in

REVIEW 2 major objections 2 minor 1 cited by

Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions

T0 review · 2 major / 2 minor · reviewed 2026-05-21 · grok-4.3

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Oblique collisions between magnetized filaments form compressed clouds whose collapse or expansion is set by the angle and an immediate energy balance check.

desk verdict The simulations map how oblique angles make filament collisions more likely to collapse, with an energy comparison right after impact as the predictor, but continued accretion could shift the outcome later. read the letter →

arxiv 2605.20835 v1 pith:2KFJNLSW submitted 2026-05-20 astro-ph.GA

Raiga Kashiwagi , Kazunari Iwasaki , Kohji Tomisaka , Tsuyoshi Inoue This is my paper · ORCID
classification astro-ph.GA
keywords filamentcollisionsobliquemagnetohydrodynamicsgravitationalcollapsemolecularcloudshub-filamentsystemsstarformation
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper runs three-dimensional ideal magnetohydrodynamical simulations of two identical finite-length magnetized filaments colliding obliquely. It varies the angle between their long axes, the collision velocity perpendicular to those axes, and the initial line mass. As the angle decreases from orthogonal toward parallel, the resulting compressed cloud becomes more prone to gravitational collapse. The authors tie this outcome directly to energies measured right after the collision: collapse occurs when the absolute gravitational energy exceeds the sum of kinetic, thermal, and magnetic energies; otherwise the cloud expands. This supplies a criterion for when filament mergers can produce the dense hubs linked to cluster and massive star formation.

What carries the argument

The instantaneous energy balance: absolute gravitational energy compared against the sum of kinetic, thermal, and magnetic energies, evaluated right after the oblique collision.

What would settle it

A simulation or observation showing a post-collision cloud where the absolute gravitational energy exceeds the sum of the other energies yet the cloud expands, or where the energies suggest expansion yet collapse occurs.

Watch

Extended reading notes

Core claim

The gravitational stability of the post-collision compressed cloud is determined by its energy balance immediately after the collision. When the absolute value of the gravitational energy exceeds the sum of the kinetic, thermal, and magnetic energies, the cloud undergoes gravitational collapse; when the gravitational energy is smaller, the cloud expands.

Load-bearing premise

The long-term gravitational stability of the compressed cloud is fully determined by comparing energies at one instant immediately after the collision, without needing to track continued accretion, magnetic field evolution, or radiative cooling over longer times.

Editorial extensions

If this is right

  • Smaller collision angles make the compressed cloud more likely to collapse gravitationally.
  • An upper limit exists on collision velocity beyond which hub-filament systems do not form.
  • The identified conditions point to collision geometries favorable for massive star formation.
  • The energy criterion offers a direct test for whether observed filament intersections will form dense hubs.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Observed alignments of filaments in molecular clouds could be used to forecast which junctions will form stars.
  • Adding radiative cooling or ongoing accretion in future runs would test how durable the single-moment energy test remains.
  • The same balance idea might extend to mergers among three or more filaments inside larger hub systems.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 2 minor

Summary. The manuscript uses 3D ideal MHD simulations of oblique collisions between two identical finite-length magnetized filaments, varying collision angle, velocity (perpendicular to the axes), and initial line mass. It reports that smaller collision angles increase the likelihood of gravitational collapse in the compressed cloud. The central result is an energy-balance criterion: the cloud collapses if |E_grav| exceeds the sum of kinetic, thermal, and magnetic energies evaluated immediately after the collision, and expands otherwise. The work also derives an upper limit on collision velocity for hub-filament formation and identifies parameter regimes favorable for massive star formation.

Significance. If the instantaneous energy criterion is robust, the paper supplies a simple, falsifiable diagnostic for predicting collapse versus expansion in filament-coalescence events, directly relevant to hub-filament systems and clustered star formation. The systematic exploration of angle, velocity, and line mass in MHD runs is a clear strength, as is the explicit linkage between simulation outcomes and an energy-based explanation.

major comments (2)
  1. [§4] §4 (energy-balance analysis): The central claim that the sign of |E_grav| − (E_kin + E_therm + E_mag) evaluated immediately after collision determines long-term collapse or expansion is load-bearing, yet the manuscript does not report time series of the four energy terms beyond that single snapshot. Because the filaments are finite, post-collision accretion continues to alter the mass distribution and E_grav on comparable timescales; without showing that the initial inequality remains decisive, the criterion’s predictive power is not fully demonstrated.
  2. [§2–3] Methods (§2–3): The simulations employ ideal MHD and therefore omit radiative cooling. The paper should quantify how the absence of cooling affects the thermal-energy term in the balance and whether the reported threshold would shift under more realistic thermodynamics, since cooling directly reduces pressure support on the same timescales as the reported collapse.
minor comments (2)
  1. Define the precise instant used for the post-collision energy evaluation (e.g., time when the filament axes have fully overlapped or a fixed multiple of the crossing time).
  2. Add panel labels or a table summarizing the exact (angle, velocity, line-mass) values for each run shown in the figures.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments and positive evaluation of our study on oblique filament collisions. We address each major point below and have revised the manuscript to improve the presentation of our results.

read point-by-point responses

  1. Referee: [§4] §4 (energy-balance analysis): The central claim that the sign of |E_grav| − (E_kin + E_therm + E_mag) evaluated immediately after collision determines long-term collapse or expansion is load-bearing, yet the manuscript does not report time series of the four energy terms beyond that single snapshot. Because the filaments are finite, post-collision accretion continues to alter the mass distribution and E_grav on comparable timescales; without showing that the initial inequality remains decisive, the criterion’s predictive power is not fully demonstrated.

    Authors: We agree that time series would strengthen the demonstration. Our existing simulations already evolve the systems for multiple free-fall times post-collision, with outcomes matching the immediate post-collision energy balance. To directly address ongoing accretion in finite filaments, the revised manuscript now includes time-evolution plots of all four energy components for representative runs. These confirm that the sign of the difference at the post-collision snapshot remains predictive and is not reversed by later mass accretion on the relevant timescales. revision: yes

  2. Referee: [§2–3] Methods (§2–3): The simulations employ ideal MHD and therefore omit radiative cooling. The paper should quantify how the absence of cooling affects the thermal-energy term in the balance and whether the reported threshold would shift under more realistic thermodynamics, since cooling directly reduces pressure support on the same timescales as the reported collapse.

    Authors: We acknowledge that omitting radiative cooling overestimates thermal support in our ideal MHD runs. Cooling would lower the thermal energy term, making gravitational collapse more likely and potentially shifting the velocity or angle thresholds. A quantitative assessment would require new simulations incorporating a cooling function, which lies outside the scope of this work focused on magnetic and geometric effects. The revised manuscript adds a dedicated paragraph in the discussion noting this limitation and stating that our reported criterion is therefore conservative. revision: partial

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: energy criterion is empirical observation from simulations

full rationale

The paper runs 3D ideal MHD simulations of oblique filament collisions across a parameter space of angles, velocities, and line masses. The central claim—that collapse occurs precisely when |E_grav| exceeds the sum of kinetic + thermal + magnetic energies evaluated immediately after collision—is presented as a finding extracted from inspecting the simulated states and their subsequent evolution. No parameter is fitted to the outcomes and then relabeled as a prediction; the energies are computed directly from the post-collision snapshot and checked against the long-term behavior within the same runs. No self-citation chain, uniqueness theorem, or ansatz smuggling is used to justify the criterion. The result is therefore self-contained as a numerical correlation rather than a tautological reduction of the output to the input.

Assumptions & free parameters 3 free parameters · 2 assumptions · 0 invented entities

The work relies on ideal MHD, identical initial filaments, and the assumption that energy balance at one post-collision time slice governs long-term fate. No new particles or forces are introduced.

free parameters (3)
  • collision angle
    Varied parametrically; not fitted but chosen to span orthogonal to parallel regimes.
  • collision velocity
    Varied parametrically; upper limit for hub formation is estimated from runs.
  • initial line mass
    Varied parametrically as a model parameter for filament properties.
assumptions (2)
  • domain assumption Ideal magnetohydrodynamics applies with no resistivity or non-ideal effects.
    Stated in abstract as three-dimensional ideal magnetohydrodynamical simulations.
  • domain assumption Two filaments are identical and finite-length with uniform properties along their axes.
    Described as model of initial filaments in the abstract.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions." pith.science (2026). https://pith.science/paper/2KFJNLSW

@misc{pith2026260520835,
  author       = {Pith},
  title        = {Pith review of: Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2KFJNLSW}},
  note         = {Machine review of arXiv:2605.20835}
}
read the original abstract

Stars are thought to form predominantly within filamentary molecular clouds. Recent studies have suggested that active star formation, including the formation of stellar clusters and massive stars, occurs within so-called "hub" structures, where multiple filaments converge. Understanding the formation and evolution of such hub-filament systems is therefore essential for unveiling the physical processes responsible for cluster and massive star formation, although the full picture remains incomplete. To address this, we have focused on filament-filament collisions as a potential formation mechanism of the hubs. In this study, we investigate the fundamental evolutionary processes of oblique collisions between two magnetized filaments using three-dimensional ideal magnetohydrodynamical simulations. As a model of initial filaments, we consider two identical finite-length magnetized filaments, varying the collision angle between their long axes, the collision velocity, which is set perpendicular to the long axes, and the initial line mass. We find that as the collision angle decreases from orthogonal to parallel, the compressed cloud becomes more prone to gravitational collapse. In addition, the instability of the post-collision compressed cloud can be explained by its energy balance. Specifically, if the absolute value of the gravitational energy exceeds the sum of the kinetic, thermal, and magnetic energies immediately after the collision, the cloud undergoes gravitational collapse. Conversely, if the gravitational energy is smaller, the cloud expands. In addition, we estimate the upper limit of the collision velocity that enables hub-filament formation and identify the collision conditions favorable for massive star formation.

Figures

Figures reproduced from arXiv: 2605.20835 by the authors.

Figure 1
Figure 1. An example of the initial condition for oblique collisions. The sim￾ulation domain is a cubic box with a side length of Lbox = 2.2 pc (i.e., x = y = z = 2.2 pc). Each filament is initially in magnetohydrostatic equi￾librium. The angle between the major axes of the filaments is denoted by θ. Magnetic field lines (black lines) are globally aligned along the x-axis, and the initial speed (Vint) is also given in the x-d… view at source ↗
Figure 2
Figure 2. Time evolution of the maximum density. The vertical axis rep￾resents the maximum density, and the horizontal axis shows time. The model parameters are λ0 = 0.5λcrit,B, and θ = π/3. The thick red line corresponds to the initial speed Vint = 0.5cs, the blue line to Vint = cs, the orange line to Vint = 4.0cs, the green line to Vint = 6.5cs, and the brown line to Vint = 8.0cs. In addition, te corresponds to the time whe… view at source ↗
Figure 3
Figure 3. Evolution of the collapse mode. Two-dimensional slices of the result of model L05V02th60 (λ0 = 0.5λcrit,B, Vint = cs, and θ = π/3). From top to bottom, each row shows slices in the z = 0, y = 0, and x = 0 planes, respectively. From left to right, the columns correspond to three representative epochs: t = 0.16Myr, 0.38Myr, and 0.49Myr. The color scale indicates the density, and the white lines represent the magnetic … view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Same as figure 3, but for the expansion mode. This figure shows results from model L05V16th60 (λ0 = 0.5λcrit,B, Vint = 8.0cs, and θ = π/3). From left to right, columns correspond to three representative epochs: t = 0.26Myr, 0.75Myr, and 1.63Myr. Alt text: A set of two-…
Figure 5
Figure 5. Figure 5: Final outcomes of oblique collisions, shown on the Vint–λ0/λcrit,B plane. Panels (a), (b), and (c) correspond to collision angles of θ = π/2, π/3, and π/6, respectively. Star symbols indicate collapse modes, while square symbols represent expansion modes. The dash-dott…
Figure 6
Figure 6. Figure 6: Relationship between the collision angle and the mass of the com￾pressed cloud. The vertical axis represents the mass of the compressed cloud, and the horizontal axis indicates the collision angle. The model pa￾rameters are fixed at λ0 = 0.5λcrit,B, and Vint = 6.5cs, w…
Figure 7
Figure 7. Figure 7: Same as figure 5, but for the different β0. The upper and lower rows correspond to the results for β0 = 1 (i.e., B0 = 6µG) and β0 = 0.01 (i.e., B0 = 60µG), respectively, while the left-to-right panels show the results for θ = π/2, θ = π/3, and θ = π/6, respectively. Fo…
Figure 8
Figure 8. Figure 8: Schematic view of the non-colliding segment on the x = 0 plane. The non-colliding segments move forward or backward along the line of sight at a velocity of Vint. One of them is illustrated as the red trapezoid, whose center of mass is located at (Cy ,Cz). Alt text: A …

Discussion (0). Continue with ORCID to comment.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. An ALMA study of hub-filament systems II.Quiescent filaments converging towards highly dynamic hubs

    astro-ph.GA 2026-08 conditional novelty 6.0 of 10

    N2H+ observations of six infrared-dark hub-filament systems show quiescent filaments converging toward dynamically complex hubs, with similar centroid velocity spreads across clumps spanning a factor of about 20 in mass.

Reference graph

Works this paper leans on

225 extracted references · 225 canonical work pages · cited by 1 Pith paper

  1. [1]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page Pith review arXiv doi:10.3847/1538-3881/aabc4f

  2. [2]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. 2013. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page Pith review arXiv doi:10.1051/0004-6361/201322068 2013

  3. [3]

    , keywords =

    SExtractor: Software for source extraction. , keywords =. 1996. doi:10.1051/aas:1996164 , adsurl =

    work page doi:10.1051/aas:1996164 1996

  4. [4]

    Quantifying the Observational Effort Required for the Radial Velocity Characterization of TESS Planets

    Quantifying the Observational Effort Required for the Radial Velocity Characterization of TESS Planets. , keywords =. 2018. doi:10.3847/1538-3881/aacea9 , archivePrefix =. 1807.01263 , primaryClass =

    work page Pith review arXiv doi:10.3847/1538-3881/aacea9 2018

  5. [5]

    X-ray Scattering Echoes and Ghost Halos from the Intergalactic Medium: Relation to the nature of AGN variability

    X-Ray Scattering Echoes and Ghost Halos from the Intergalactic Medium: Relation to the Nature of AGN Variability. , keywords =. 2015. doi:10.1088/0004-637X/805/1/23 , archivePrefix =. 1503.01475 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/805/1/23 2015

  6. [6]

    , keywords =

    The 2013 Release of Cloudy. , keywords =. 2013

    work page 2013

  7. [7]

    1989", month =

    T _ E X and LAT _ E X Macro Definition Files for Astronomical Publications. , year = "1989", month = "Mar", pages =

    work page 1989

  8. [8]

    LaTeX: A Document Preparation System. 1994

    work page 1994

Show all 225 references
  1. [9]

    , keywords =

    Quasi-periodic Fast Propagating Magnetoacoustic Waves during the Magnetic Reconnection Between Solar Coronal Loops. , keywords =. 2018. doi:10.3847/2041-8213/aaf167 , archivePrefix =. 1811.08553 , primaryClass =

    2018 doi arXiv

  2. [10]

    , keywords =

    Nominal Values for Selected Solar and Planetary Quantities: IAU 2015 Resolution B3. , keywords =. 2016. doi:10.3847/0004-6256/152/2/41 , archivePrefix =. 1605.09788 , primaryClass =

    2015 doi arXiv

  3. [11]

    Swift X-Ray Observations of Classical Novae. II. The Super Soft Source Sample. , keywords =. 2011. doi:10.1088/0067-0049/197/2/31 , archivePrefix =. 1110.6224 , primaryClass =

    2011 doi arXiv

  4. [12]

    , keywords =

    Galaxy Emission Line Classification Using Three-dimensional Line Ratio Diagrams. , keywords =. 2014. doi:10.1088/0004-637X/793/2/127 , archivePrefix =. 1406.5186 , primaryClass =

    2014 doi arXiv

  5. [13]

    Lemuridae , abstract =

    Behrens, Ken and Barnes, Keith , month = dec, year =. Lemuridae , abstract =. Wildlife of. doi:10.1515/9781400880676-008 , pages =

    doi

  6. [14]

    , year =

    Heard, Stephen B. , year =. Charles

  7. [15]

    Science Fiction Studies , author =

    The. Science Fiction Studies , author =. 1979 , pages =

    1979

  8. [16]

    Poetry , author =

    Lemur. Poetry , author =. 1996 , pages =

    1996

  9. [17]

    , year =

    Wright, Patricia C. , year =. For the

  10. [18]

    McGoogan, Keriann , year =. Chasing

  11. [19]

    , keywords =

    Magnetohydrostatic Equilibrium Structure and Mass of Filamentary Isothermal Cloud Threaded by Lateral Magnetic Field. , keywords =. doi:10.1088/0004-637X/785/1/24 , archivePrefix =. 1402.3033 , primaryClass =

    doi arXiv

  12. [20]

    Part III

    On the Gravitational Instability of Some Magneto-Hydrodynamical Systems of Astrophysical Interest. Part III. Acta Astronomica , keywords =

  13. [21]

    , keywords =

    SCUBA and Spitzer observations of the Taurus molecular cloud - pulling the bull's tail. , keywords =. doi:10.1111/j.1365-2966.2007.12750.x , archivePrefix =. 0711.3565 , primaryClass =

    2007 doi

  14. [22]

    Structure and stability

    Polytropic models of filamentary interstellar clouds - I. Structure and stability. , keywords =. doi:10.1093/mnras/stu2168 , archivePrefix =. 1410.6091 , primaryClass =

    doi arXiv

  15. [23]

    , keywords =

    Characterizing interstellar filaments with Herschel in IC 5146. , keywords =. doi:10.1051/0004-6361/201116596 , archivePrefix =. 1103.0201 , primaryClass =

    doi arXiv

  16. [24]

    , keywords =

    Gravitational Collapse of Filamentary Clouds. , keywords =. doi:10.1093/pasj/50.6.577 , adsurl =

    doi

  17. [25]

    , keywords =

    Characterizing the properties of nearby molecular filaments observed with Herschel. , keywords =. doi:10.1051/0004-6361/201832725 , archivePrefix =. 1810.00721 , primaryClass =

    doi arXiv

  18. [26]

    , keywords =

    Herschel view of the Taurus B211/3 filament and striations: evidence of filamentary growth?. , keywords =. doi:10.1051/0004-6361/201220500 , archivePrefix =. 1211.6360 , primaryClass =

    doi arXiv

  19. [27]

    , year = 1964, month = oct, volume =

    The Equilibrium of Polytropic and Isothermal Cylinders. , year = 1964, month = oct, volume =. doi:10.1086/148005 , adsurl =

    1964 doi

  20. [28]

    , keywords =

    Near-infrared-imaging Polarimetry Toward Serpens South: Revealing the Importance of the Magnetic Field. , keywords =. doi:10.1088/0004-637X/734/1/63 , archivePrefix =. 1104.2977 , primaryClass =

    doi arXiv

  21. [29]

    , keywords =

    The Magnetic Field in Taurus Probed by Infrared Polarization. , keywords =. doi:10.1088/0004-637X/741/1/21 , archivePrefix =. 1108.0410 , primaryClass =

    doi arXiv

  22. [30]

    , keywords =

    Polarization Structure of Filamentary Clouds. , keywords =. doi:10.1088/0004-637X/807/1/47 , archivePrefix =. 1505.02895 , primaryClass =

    doi arXiv

  23. [31]

    Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds. , keywords =. doi:10.1051/0004-6361/201525896 , archivePrefix =. 1502.04123 , primaryClass =

    doi arXiv

  24. [32]

    , keywords =

    The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333. , keywords =. doi:10.3847/1538-4357/aba1e2 , archivePrefix =. 2007.00176 , primaryClass =

    2007 doi

  25. [33]

    , keywords =

    From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey. , keywords =. doi:10.1051/0004-6361/201014666 , archivePrefix =. 1005.2618 , primaryClass =

    doi arXiv

  26. [34]

    An ESA facility for far-infrared and submillimetre astronomy

    Herschel Space Observatory. An ESA facility for far-infrared and submillimetre astronomy. , keywords =. doi:10.1051/0004-6361/201014759 , archivePrefix =. 1005.5331 , primaryClass =

    doi arXiv

  27. [35]

    , keywords =

    Filamentary structures and compact objects in the Aquila and Polaris clouds observed by Herschel. , keywords =. doi:10.1051/0004-6361/201014668 , archivePrefix =. 1005.3115 , primaryClass =

    doi arXiv

  28. [36]

    , keywords =

    A Herschel study of the properties of starless cores in the Polaris Flare dark cloud region using PACS and SPIRE. , keywords =. doi:10.1051/0004-6361/201014618 , archivePrefix =. 1005.2519 , primaryClass =

    doi arXiv

  29. [37]

    , keywords =

    Magnetic field structure in the Taurus dark cloud. , keywords =. doi:10.1086/162228 , adsurl =

    doi

  30. [38]

    , keywords =

    Expanded Very Large Array Observations of the Barnard 5 Star-forming Core: Embedded Filaments Revealed. , keywords =. doi:10.1088/2041-8205/739/1/L2 , archivePrefix =. 1106.5474 , primaryClass =

    doi arXiv

  31. [39]

    , keywords =

    Initial Conditions for Star Formation in Clusters: Physical and Kinematical Structure of the Starless Core Oph A-N6. , keywords =. doi:10.1088/0004-637X/745/2/117 , archivePrefix =. 1111.4424 , primaryClass =

    doi arXiv

  32. [40]

    , keywords =

    L1495 revisited: a PPMAP view of a star-forming filament. , keywords =. doi:10.1093/mnras/stz2234 , archivePrefix =. 1908.02295 , primaryClass =

    1908 doi

  33. [41]

    , keywords =

    Dense core formation by fragmentation of velocity-coherent filaments in L1517. , keywords =. doi:10.1051/0004-6361/201117039 , archivePrefix =. 1107.0971 , primaryClass =

    doi arXiv

  34. [42]

    Planck intermediate results. XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps. , keywords =. doi:10.1051/0004-6361/201425305 , archivePrefix =. 1411.2271 , primaryClass =

    doi arXiv

  35. [43]

    , keywords =

    Magnetic fields in star-forming systems (II): examining dust polarization, the Zeeman effect, and the Faraday rotation measure as magnetic field tracers. , keywords =. doi:10.1093/mnras/staa3148 , archivePrefix =. 2009.04201 , primaryClass =

    2009 doi

  36. [44]

    , keywords =

    Magnetic Field of the Vela C Molecular Cloud. , keywords =. doi:10.3847/2041-8205/830/2/L23 , adsurl =

    doi

  37. [45]

    , keywords =

    Relative Alignment between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud Using Low- and High-density Tracers. , keywords =. doi:10.3847/1538-4357/ab1eb0 , archivePrefix =. 1804.08979 , primaryClass =

    doi arXiv

  38. [46]

    , keywords =

    The relation between the column density structures and the magnetic field orientation in the Vela C molecular complex. , keywords =. doi:10.1051/0004-6361/201730608 , archivePrefix =. 1702.03853 , primaryClass =

    doi arXiv

  39. [47]

    , year = 1974, month = jul, volume =

    Polytropic Sheets, Cylinders and Spheres with Negative Index. , year = 1974, month = jul, volume =

    1974

  40. [48]

    , year = 1969, month = jan, volume =

    Numerical calculations of the dynamics of collapsing proto-star. , year = 1969, month = jan, volume =. doi:10.1093/mnras/145.3.271 , adsurl =

    1969 doi

  41. [49]

    An introduction to the study of stellar structure

  42. [50]

    Helical magnetic fields

    Polytropic models of filamentary interstellar clouds - II. Helical magnetic fields. , keywords =. doi:10.1093/mnras/stu2194 , archivePrefix =. 1410.6092 , primaryClass =

    doi arXiv

  43. [51]

    Protostars and Planets VI , year = 2014, editor =

    From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation. Protostars and Planets VI , year = 2014, editor =. doi:10.2458/azu_uapress_9780816531240-ch002 , archivePrefix =. 1312.6232 , primaryClass =

    2014 doi arXiv

  44. [52]

    Frontiers in Astronomy and Space Sciences , keywords =

    The role of magnetic field in molecular cloud formation and evolution. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2019.00005 , archivePrefix =. 1902.00798 , primaryClass =

    2019 doi

  45. [53]

    , year = 1958, month = jan, volume =

    Stability of polytropic gas spheres. , year = 1958, month = jan, volume =. doi:10.1093/mnras/118.5.523 , adsurl =

    1958 doi

  46. [54]

    Progress of Theoretical Physics , year = 1987, month = mar, volume =

    Gravitational Instability of the Isothermal Gas Cylinder with an Axial magnetic Field. Progress of Theoretical Physics , year = 1987, month = mar, volume =. doi:10.1143/PTP.77.635 , adsurl =

    1987 doi

  47. [55]

    , keywords =

    Self-similar Solutions and the Stability of Collapsing Isothermal Filaments. , keywords =. doi:10.1086/171162 , adsurl =

    doi

  48. [56]

    , keywords =

    Helical fields and filamentary molecular clouds - I. , keywords =. doi:10.1046/j.1365-8711.2000.03066.x , archivePrefix =. astro-ph/9901096 , primaryClass =

    2000 doi

  49. [57]

    , keywords =

    The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers. , keywords =. doi:10.3847/1538-4365/ab929b , archivePrefix =. 2005.06651 , primaryClass =

    2005 doi

  50. [58]

    , keywords =

    The Jeans Condition: A New Constraint on Spatial Resolution in Simulations of Isothermal Self-gravitational Hydrodynamics. , keywords =. doi:10.1086/310975 , adsurl =

    doi

  51. [59]

    Journal of Computational Physics , year = 2005, month = sep, volume =

    A multi-state HLL approximate Riemann solver for ideal magnetohydrodynamics. Journal of Computational Physics , year = 2005, month = sep, volume =. doi:10.1016/j.jcp.2005.02.017 , adsurl =

    2005 doi

  52. [60]

    Journal of Scientific Computing , year = 2009, month = mar, volume =

    High Order Strong Stability Preserving Time Discretizations. Journal of Scientific Computing , year = 2009, month = mar, volume =. doi:10.1007/s10915-008-9239-z , adsurl =

    2009 doi

  53. [61]

    , keywords =

    Athena: A New Code for Astrophysical MHD. , keywords =. doi:10.1086/588755 , archivePrefix =. 0804.0402 , primaryClass =

    doi arXiv

  54. [62]

    , keywords =

    An Origin of Filamentary Structure in Molecular Clouds. , keywords =. doi:10.1086/306249 , adsurl =

    doi

  55. [63]

    , keywords =

    Cluster Formation Triggered by Filament Collisions in Serpens South. , keywords =. doi:10.1088/2041-8205/791/2/L23 , archivePrefix =. 1407.1235 , primaryClass =

    doi arXiv

  56. [64]

    The highest mass stars (>100 M _ ) form only in hubs

    Unifying low- and high-mass star formation through density-amplified hubs of filaments. The highest mass stars (>100 M _ ) form only in hubs. , keywords =. doi:10.1051/0004-6361/202038232 , archivePrefix =. 2008.00295 , primaryClass =

    2008 doi

  57. [65]

    , keywords =

    Was a cloud-cloud collision the trigger of the recent star formation in Serpens?. , keywords =. doi:10.1051/0004-6361/201015477 , archivePrefix =. 1101.2412 , primaryClass =

    doi arXiv

  58. [66]

    , keywords =

    Merging filaments I: a race against collapse. , keywords =. doi:10.1093/mnras/stab1698 , archivePrefix =. 2104.04541 , primaryClass =

    doi

  59. [67]

    , keywords =

    A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey. , keywords =. doi:10.1051/0004-6361/201525861 , archivePrefix =. 1507.05926 , primaryClass =

    doi arXiv

  60. [68]

    , keywords =

    Properties of the dense core population in Orion B as seen by the Herschel Gould Belt survey. , keywords =. doi:10.1051/0004-6361/201834753 , archivePrefix =. 1910.04053 , primaryClass =

    1910 doi

  61. [69]

    , keywords =

    Near-infrared imaging polarimetry toward M 17 SWex. , keywords =. doi:10.1093/pasj/psz072 , archivePrefix =. 1906.12138 , primaryClass =

    1906 doi

  62. [70]

    BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network

    Dust polarized emission observations of NGC 6334. BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network. , keywords =. doi:10.1051/0004-6361/202038624 , archivePrefix =. 2012.13060 , primaryClass =

    2012 doi

  63. [71]

    , keywords =

    Simulation of Magnetohydrodynamic Flows: A Constrained Transport Model. , keywords =. doi:10.1086/166684 , adsurl =

    doi

  64. [72]

    II ---Full Nonlinear Numerical Simulations---

    Fragmentation of Isothermal Sheet-Like Clouds. II ---Full Nonlinear Numerical Simulations---. Progress of Theoretical Physics , year = 1987, month = dec, volume =. doi:10.1143/PTP.78.1273 , adsurl =

    1987 doi

  65. [73]

    , year = 1978, month = jan, volume =

    Gravitational Instability of Magnetized Gaseous Disks 6. , year = 1978, month = jan, volume =

    1978

  66. [74]

    , keywords =

    The Cluster-forming Site AFGL 5157: Colliding Filamentary Clouds and Star Formation. , keywords =. doi:10.3847/1538-4357/ab4189 , archivePrefix =. 1909.01298 , primaryClass =

    1909 doi

  67. [75]

    Correlation of density, kinematics, and magnetic field in the Pipe nebula

    Formation of dense structures induced by filament collisions. Correlation of density, kinematics, and magnetic field in the Pipe nebula. , keywords =. doi:10.1051/0004-6361/201425234 , archivePrefix =. 1412.4778 , primaryClass =

    doi arXiv

  68. [76]

    , keywords =

    Filamentary Structure of Star-forming Complexes. , keywords =. doi:10.1088/0004-637X/700/2/1609 , archivePrefix =. 0906.2005 , primaryClass =

    2005 doi arXiv

  69. [77]

    Two very different sub-(proto)clusters

    The physical and dynamical structure of Serpens. Two very different sub-(proto)clusters. , keywords =. doi:10.1051/0004-6361/200913919 , archivePrefix =. 1006.0879 , primaryClass =

    doi arXiv

  70. [78]

    , keywords =

    Magnetic braking of an aligned rotator during star formation - an exact, time-dependent solution. , keywords =. doi:10.1086/157936 , adsurl =

    doi

  71. [79]

    , keywords =

    The Evolution of the Angular Momentum Distribution during Star Formation. , keywords =. doi:10.1086/312417 , archivePrefix =. astro-ph/9911166 , primaryClass =

    doi arXiv

  72. [80]

    , keywords =

    Simulations of Magnetohydrodynamic Turbulence in a Strongly Magnetized Medium. , keywords =. doi:10.1086/324186 , archivePrefix =. astro-ph/0105235 , primaryClass =

    doi arXiv

  73. [81]

    , keywords =

    Formation of Turbulent and Magnetized Molecular Clouds via Accretion Flows of H I Clouds. , keywords =. doi:10.1088/0004-637X/759/1/35 , archivePrefix =. 1205.6217 , primaryClass =

    doi arXiv

  74. [82]

    , keywords =

    Universal Properties of Dense Clumps in Magnetized Molecular Clouds Formed through Shock Compression of Two-phase Atomic Gases. , keywords =. doi:10.3847/1538-4357/ac75cc , archivePrefix =. 2206.03627 , primaryClass =

    doi

  75. [83]

    , keywords =

    Magnetohydrostatic Equilibrium Structure and Mass of Polytropic Filamentary Cloud Threaded by Lateral Magnetic Field. , keywords =. doi:10.3847/1538-4357/abea7a , archivePrefix =. 2103.02846 , primaryClass =

    doi

  76. [84]

    , keywords =

    Gravitational Collapse of Isothermal Magnetized Clouds: The Universality of Self-similar Collapse. , keywords =. doi:10.1086/306553 , adsurl =

    doi

  77. [85]

    Journal of Computational Physics , keywords =

    An unsplit Godunov method for ideal MHD via constrained transport. Journal of Computational Physics , keywords =. doi:10.1016/j.jcp.2004.11.016 , archivePrefix =. astro-ph/0501557 , primaryClass =

    2004 doi arXiv

  78. [86]

    Journal of Computational Physics , keywords =

    An unsplit Godunov method for ideal MHD via constrained transport in three dimensions. Journal of Computational Physics , keywords =. doi:10.1016/j.jcp.2007.12.017 , archivePrefix =. 0712.2634 , primaryClass =

    2007 doi arXiv

  79. [87]

    An origin for the cloud mass function and star formation efficiency

    The formation and destruction of molecular clouds and galactic star formation. An origin for the cloud mass function and star formation efficiency. , keywords =. doi:10.1051/0004-6361/201425584 , archivePrefix =. 1505.04696 , primaryClass =

    doi arXiv

  80. [88]

    , keywords =

    Gravitational instability of isothermal gas layers - Effect of curvature and magnetic field. , keywords =

  81. [89]

    An ALMA View of Molecular Filaments in the Large Magellanic Cloud. II. An Early Stage of High-mass Star Formation Embedded at Colliding Clouds in N159W-South. , keywords =. doi:10.3847/1538-4357/ab48ff , archivePrefix =. 1811.04400 , primaryClass =

    doi

  82. [90]

    , keywords =

    The Star Formation Rate of Turbulent Magnetized Clouds: Comparing Theory, Simulations, and Observations. , keywords =. doi:10.1088/0004-637X/761/2/156 , archivePrefix =. 1209.2856 , primaryClass =

    doi arXiv

  83. [91]

    , keywords =

    Formation of Massive Molecular Cloud Cores by Cloud-Cloud Collision. , keywords =. doi:10.1088/2041-8205/774/2/L31 , archivePrefix =. 1305.4655 , primaryClass =

    doi arXiv

  84. [92]

    arXiv e-prints , keywords =

    The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-Gravity. arXiv e-prints , keywords =

  85. [93]

    Fragmentation of a Filamentary Cloud Permeated by a Perpendicular Magnetic Field. II. Dependence on the Initial Density Profile. , keywords =. doi:10.3847/1538-4357/ab2d26 , archivePrefix =. 1907.03384 , primaryClass =

    1907 doi

  86. [94]

    , keywords =

    Fragmentation of a Filamentary Cloud Permeated by a Perpendicular Magnetic Field. , keywords =. doi:10.3847/1538-4357/aa8b6d , archivePrefix =. 1709.05149 , primaryClass =

    doi arXiv

  87. [95]

    , keywords =

    Effects of Magnetic Fields and Rotation on the Fragmentation of Filamentary Molecular Clouds: Comparison of the Theory with the Orion A Cloud. , keywords =. doi:10.1086/186749 , adsurl =

    doi

  88. [96]

    , keywords =

    Fragmentation of Filamentary Molecular Clouds with Longitudinal and Helical Magnetic Fields. , keywords =

  89. [97]

    Axisymmetric stability and fragmentation

    Helical fields and filamentary molecular clouds - II. Axisymmetric stability and fragmentation. , keywords =. doi:10.1046/j.1365-8711.2000.03067.x , archivePrefix =. astro-ph/9902385 , primaryClass =

    doi

  90. [98]

    Nature Astronomy , keywords =

    Magnetized filamentary gas flows feeding the young embedded cluster in Serpens South. Nature Astronomy , keywords =. doi:10.1038/s41550-020-1172-6 , archivePrefix =. 2009.14100 , primaryClass =

    2009 doi

  91. [99]

    , keywords =

    Magnetic field structure in Serpens South. , keywords =. doi:10.1093/pasj/psz040 , adsurl =

    doi

  92. [100]

    , keywords =

    The Dynamical State of the Serpens South Filamentary Infrared Dark Cloud. , keywords =. doi:10.1088/0004-637X/778/1/34 , archivePrefix =. 1309.2425 , primaryClass =

    doi arXiv

  93. [101]

    Physical Review , year = 1951, month = mar, volume =

    The Strength of Interstellar Magnetic Fields. Physical Review , year = 1951, month = mar, volume =. doi:10.1103/PhysRev.81.890.2 , adsurl =

    1951 doi

  94. [102]

    , year = 1953, month = jul, volume =

    Magnetic Fields in Spiral Arms. , year = 1953, month = jul, volume =. doi:10.1086/145731 , adsurl =

    1953 doi

  95. [103]

    , keywords =

    Clump collisions in molecular clouds - Gravitational instability and coalescence. , keywords =. doi:10.1086/161894 , adsurl =

    doi

  96. [104]

    I ---Head-On Collisions---

    Three-Dimensional Numerical Simulation of Interstellar Cloud-Cloud Collisions and Triggered Star Formation. I ---Head-On Collisions---. Progress of Theoretical Physics , year = 1987, month = dec, volume =. doi:10.1143/PTP.78.1250 , adsurl =

    1987 doi

  97. [105]

    , year = 1956, month = jan, volume =

    Boyle's Law and gravitational instability. , year = 1956, month = jan, volume =. doi:10.1093/mnras/116.3.351 , adsurl =

    1956 doi

  98. [106]

    Mit 5 Textabbildungen

    \"U ber die Verdichtung von H I-Gebieten. Mit 5 Textabbildungen. , year = 1955, month = jan, volume =

    1955

  99. [107]

    , keywords =

    Fragmentation and mass segregation in the massive dense cores of Cygnus X. , keywords =. doi:10.1051/0004-6361/200913286 , archivePrefix =. 0909.2315 , primaryClass =

    doi arXiv

  100. [108]

    , keywords =

    Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way. , keywords =. doi:10.1051/0004-6361/201014659 , archivePrefix =. 1005.3317 , primaryClass =

    doi arXiv

  101. [109]

    , keywords =

    The Hi-GAL catalogue of dusty filamentary structures in the Galactic plane. , keywords =. doi:10.1093/mnras/stz3466 , archivePrefix =. 1912.04020 , primaryClass =

    1912 doi

  102. [110]

    , keywords =

    ATLASGAL: A Galaxy-wide sample of dense filamentary structures. , keywords =. doi:10.1051/0004-6361/201527468 , archivePrefix =. 1604.00544 , primaryClass =

    doi arXiv

  103. [111]

    , keywords =

    SEDIGISM: Structure, excitation, and dynamics of the inner Galactic interstellar medium. , keywords =. doi:10.1051/0004-6361/201628933 , archivePrefix =. 1701.04712 , primaryClass =

    doi arXiv

  104. [112]

    , keywords =

    A census of dense cores in the Taurus L1495 cloud from the Herschel. , keywords =. doi:10.1093/mnras/stw301 , archivePrefix =. 1602.03143 , primaryClass =

    doi arXiv

  105. [113]

    Equilibria and Evolutions of Magnetized, Rotating, Isothermal Clouds. II. The Extreme Case: Nonrotating Clouds. , keywords =. doi:10.1086/166923 , adsurl =

    doi

  106. [114]

    , keywords =

    Note on the collapse of magnetic interstellar clouds. , keywords =. doi:10.1086/154835 , adsurl =

    doi

  107. [115]

    Physics of the Interstellar and Intergalactic Medium

  108. [116]

    Spiral arms as sheared gravitational instabilities

    II. Spiral arms as sheared gravitational instabilities. , year = 1965, month = jan, volume =. doi:10.1093/mnras/130.2.125 , adsurl =

    1965 doi

  109. [117]

    , keywords =

    Gravitational instability of magnetized gaseous disks. , keywords =

  110. [118]

    , keywords =

    Star formation in shock-compressed layers. , keywords =. doi:10.1086/155991 , adsurl =

    doi

  111. [119]

    , keywords =

    Global collapse of molecular clouds as a formation mechanism for the most massive stars. , keywords =. doi:10.1051/0004-6361/201321318 , archivePrefix =. 1307.2590 , primaryClass =

    doi arXiv

  112. [120]

    , keywords =

    Characterizing filaments in regions of high-mass star formation: High-resolution submilimeter imaging of the massive star-forming complex NGC 6334 with ArT \'e MiS. , keywords =. doi:10.1051/0004-6361/201628378 , archivePrefix =. 1605.07434 , primaryClass =

    doi arXiv

  113. [121]

    , keywords =

    An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud. , keywords =. doi:10.3847/1538-4357/acefb7 , archivePrefix =. 2308.05568 , primaryClass =

    doi

  114. [122]

    , keywords =

    Probing accretion of ambient cloud material into the Taurus B211/B213 filament. , keywords =. doi:10.1051/0004-6361/201834399 , archivePrefix =. 1811.06240 , primaryClass =

    doi arXiv

  115. [123]

    , keywords =

    High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22. , keywords =. doi:10.3847/1538-4357/aa9d40 , archivePrefix =. 1711.08951 , primaryClass =

    doi arXiv

  116. [124]

    , keywords =

    Probing fragmentation and velocity sub-structure in the massive NGC 6334 filament with ALMA. , keywords =. doi:10.1051/0004-6361/201935689 , archivePrefix =. 1910.02622 , primaryClass =

    1910 doi

  117. [125]

    Implications for massive star and cluster formation

    Filament coalescence and hub structure in Mon R2. Implications for massive star and cluster formation. , keywords =. doi:10.1051/0004-6361/202140363 , archivePrefix =. 2112.06803 , primaryClass =

    doi

  118. [126]

    The case of the high-mass star-forming complex Monoceros R2

    Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2. , keywords =. doi:10.1051/0004-6361/201935260 , archivePrefix =. 1907.03524 , primaryClass =

    1907 doi

  119. [127]

    , keywords =

    On the universality of interstellar filaments: theory meets simulations and observations. , keywords =. doi:10.1093/mnras/stv2880 , archivePrefix =. 1510.05654 , primaryClass =

    doi arXiv

  120. [128]

    , keywords =

    Star Formation in Turbulent Molecular Clouds with Colliding Flow. , keywords =. doi:10.1088/0004-637X/801/2/77 , archivePrefix =. 1412.5741 , primaryClass =

    doi arXiv

  121. [129]

    Gravitational Collapse in Turbulent Molecular Clouds. I. Gasdynamical Turbulence. , keywords =. doi:10.1086/308891 , archivePrefix =. astro-ph/9911068 , primaryClass =

    doi arXiv

  122. [130]

    , keywords =

    A Super-Alfv \'e nic Model of Dark Clouds. , keywords =. doi:10.1086/307956 , archivePrefix =. astro-ph/9901288 , primaryClass =

    doi arXiv

  123. [131]

    Philosophical Transactions of the Royal Society of London Series A , keywords =

    Shock interactions, turbulence and the origin of the stellar mass spectrum. Philosophical Transactions of the Royal Society of London Series A , keywords =. doi:10.1098/rsta.2012.0248 , archivePrefix =. 1201.2650 , primaryClass =

    2012 doi

  124. [132]

    , keywords =

    The Turbulent Shock Origin of Proto-Stellar Cores. , keywords =. doi:10.1086/320636 , archivePrefix =. astro-ph/0011122 , primaryClass =

    doi arXiv

  125. [133]

    , keywords =

    The responses of magnetically subcritical cores to shocks. , keywords =. doi:10.1093/mnras/stt800 , archivePrefix =. 1305.1716 , primaryClass =

    doi arXiv

  126. [134]

    , keywords =

    The formation of massive molecular filaments and massive stars triggered by a magnetohydrodynamic shock wave. , keywords =. doi:10.1093/pasj/psx089 , archivePrefix =. 1707.02035 , primaryClass =

    doi arXiv

  127. [135]

    , keywords =

    Classification of Filament Formation Mechanisms in Magnetized Molecular Clouds. , keywords =. doi:10.3847/1538-4357/ac07a1 , archivePrefix =. 2012.02205 , primaryClass =

    2012 doi

  128. [136]

    Hints from velocity dispersion measurements

    Formation and evolution of interstellar filaments. Hints from velocity dispersion measurements. , keywords =. doi:10.1051/0004-6361/201220822 , archivePrefix =. 1303.3024 , primaryClass =

    doi arXiv

  129. [137]

    , keywords =

    Opacity broadening and interpretation of suprathermal CO linewidths: Macroscopic turbulence and tangled molecular clouds. , keywords =. doi:10.1051/0004-6361/201527319 , archivePrefix =. 1603.08521 , primaryClass =

    doi arXiv

  130. [138]

    , keywords =

    A Census of Large-scale ( 10 PC), Velocity-coherent, Dense Filaments in the Northern Galactic Plane: Automated Identification Using Minimum Spanning Tree. , keywords =. doi:10.3847/0067-0049/226/1/9 , archivePrefix =. 1607.06452 , primaryClass =

    doi arXiv

  131. [139]

    , keywords =

    Dynamic star formation in the massive DR21 filament. , keywords =. doi:10.1051/0004-6361/201014481 , archivePrefix =. 1003.4198 , primaryClass =

    doi arXiv

  132. [140]

    , keywords =

    The spine of the swan: a Herschel study of the DR21 ridge and filaments in Cygnus X. , keywords =. doi:10.1051/0004-6361/201219429 , archivePrefix =. 1206.1243 , primaryClass =

    doi arXiv

  133. [141]

    , keywords =

    SDC13 infrared dark clouds: Longitudinally collapsing filaments?. , keywords =. doi:10.1051/0004-6361/201322172 , archivePrefix =. 1311.0203 , primaryClass =

    doi arXiv

  134. [142]

    Hints of multiple compressions and their impact on the cloud properties

    Velocity structure of the 50 pc long NGC 6334 filamentary cloud. Hints of multiple compressions and their impact on the cloud properties. , keywords =. doi:10.1051/0004-6361/202141699 , archivePrefix =. 2201.04267 , primaryClass =

    doi

  135. [143]

    , keywords =

    Very Large Array Observations of Ammonia in High-mass Star Formation Regions. , keywords =. doi:10.1088/0004-637X/790/2/84 , archivePrefix =. 1405.7933 , primaryClass =

    doi arXiv

  136. [144]

    , keywords =

    Structure and radial equilibrium of filamentary molecular clouds. , keywords =. doi:10.1093/mnras/stt720 , archivePrefix =. 1305.5008 , primaryClass =

    doi arXiv

  137. [145]

    , keywords =

    Physical Properties of Large-scale Galactic Filaments. , keywords =. doi:10.3847/1538-4357/aacc66 , archivePrefix =. 1712.09655 , primaryClass =

    doi arXiv

  138. [146]

    , keywords =

    OGHReS: Large-scale filaments in the outer Galaxy. , keywords =. doi:10.1051/0004-6361/202142182 , archivePrefix =. 2111.02768 , primaryClass =

    doi

  139. [147]

    , keywords =

    Large-Scale Structure of the Molecular Gas in Taurus Revealed by High Linear Dynamic Range Spectral Line Mapping. , keywords =. doi:10.1086/587166 , archivePrefix =. 0802.2206 , primaryClass =

    doi arXiv

  140. [148]

    , keywords =

    Filamentary structure and magnetic field orientation in Musca. , keywords =. doi:10.1051/0004-6361/201527068 , adsurl =

    doi

  141. [149]

    , keywords =

    First results from the Herschel Gould Belt Survey in Taurus. , keywords =. doi:10.1093/mnras/stt561 , archivePrefix =. 1304.4098 , primaryClass =

    doi arXiv

  142. [150]

    , keywords =

    Magnetically Aligned H I Fibers and the Rolling Hough Transform. , keywords =. doi:10.1088/0004-637X/789/1/82 , archivePrefix =. 1312.1338 , primaryClass =

    doi arXiv

  143. [151]

    , keywords =

    Cold Milky Way HI Gas in Filaments. , keywords =. doi:10.3847/0004-637X/821/2/117 , archivePrefix =. 1602.07604 , primaryClass =

    doi arXiv

  144. [152]

    , keywords =

    A compilation of interstellar gas properties. , keywords =. doi:10.1086/156500 , adsurl =

    doi

  145. [153]

    , keywords =

    Resolving the Vela C ridge with P-ArT \'e MiS and Herschel. , keywords =. doi:10.1051/0004-6361/201220504 , archivePrefix =. 1211.0275 , primaryClass =

    doi arXiv

  146. [154]

    The nature of the bubbles observed by Spitzer and what ATLASGAL tells us about the surrounding neutral material

    A gallery of bubbles. The nature of the bubbles observed by Spitzer and what ATLASGAL tells us about the surrounding neutral material. , keywords =. doi:10.1051/0004-6361/201014422 , archivePrefix =. 1008.0926 , primaryClass =

    doi arXiv

  147. [155]

    Bipolar H II regions. II. Morphologies and star formation in their vicinities. , keywords =. doi:10.1051/0004-6361/201833015 , adsurl =

    doi

  148. [156]

    , keywords =

    ATLASGAL - The APEX telescope large area survey of the galaxy at 870 m. , keywords =. doi:10.1051/0004-6361/200811568 , archivePrefix =. 0903.1369 , primaryClass =

    doi arXiv

  149. [157]

    , keywords =

    The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity. , keywords =. doi:10.3847/1538-4365/acc2c0 , archivePrefix =. 2302.13903 , primaryClass =

    doi

  150. [158]

    , year = 1951, month = sep, volume =

    The Polarization of Starlight by Aligned Dust Grains. , year = 1951, month = sep, volume =. doi:10.1086/145464 , adsurl =

    1951 doi

  151. [159]

    , year = 2012, month = sep, volume =

    Magnetic Fields in Molecular Clouds. , year = 2012, month = sep, volume =. doi:10.1146/annurev-astro-081811-125514 , adsurl =

    2012 doi

  152. [160]

    , keywords =

    A Production Mechanism for Clusters of Dense Cores. , keywords =. doi:10.1086/303982 , adsurl =

    doi

  153. [161]

    , keywords =

    The Aquila prestellar core population revealed by Herschel. , keywords =. doi:10.1051/0004-6361/201014689 , archivePrefix =. 1005.2981 , primaryClass =

    doi arXiv

  154. [162]

    Growth of Massive Molecular Cloud Filament by Accretion Flows. I. Slow-shock Instability versus Ambipolar Diffusion. , keywords =. doi:10.3847/1538-4357/ad072a , archivePrefix =. 2310.16448 , primaryClass =

    doi

  155. [163]

    , keywords =

    Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution. , keywords =. doi:10.3847/1538-4357/ace7bd , archivePrefix =. 2307.07698 , primaryClass =

    doi

  156. [164]

    Protostars and Planets VII , year = 2023, editor =

    Initial Conditions for Star Formation: a Physical Description of the Filamentary ISM. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2203.09562 , archivePrefix =. 2203.09562 , primaryClass =

    2023 doi

  157. [165]

    Protostars and Planets VII , year = 2023, editor =

    Magnetic Fields in Star Formation: from Clouds to Cores. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2203.11179 , archivePrefix =. 2203.11179 , primaryClass =

    2023 doi

  158. [166]

    , keywords =

    High-mass Star Formation Triggered by Collision between CO Filaments in N159 West in the Large Magellanic Cloud. , keywords =. doi:10.1088/2041-8205/807/1/L4 , archivePrefix =. 1503.03540 , primaryClass =

    doi arXiv

  159. [167]

    Ellipsoidal Figures of Equilibrium

  160. [168]

    , keywords =

    Galactic 'Snake' IRDC G11.11-0.12: a site of multiple hub-filament systems and colliding filamentary clouds. , keywords =. doi:10.1093/mnras/stad3384 , archivePrefix =. 2310.20404 , primaryClass =

    doi

  161. [169]

    , keywords =

    Insights on the Sun Birth Environment in the Context of Star Cluster Formation in Hub-Filament Systems. , keywords =. doi:10.3847/2041-8213/acc849 , archivePrefix =. 2303.15695 , primaryClass =

    doi

  162. [170]

    , keywords =

    The Formation of Massive Stars from Turbulent Cores. , keywords =. doi:10.1086/346149 , archivePrefix =. astro-ph/0206037 , primaryClass =

    doi arXiv

  163. [171]

    Journal of Computational Physics , keywords =

    Local Adaptive Mesh Refinement for Shock Hydrodynamics. Journal of Computational Physics , keywords =. doi:10.1016/0021-9991(89)90035-1 , adsurl =

    doi

  164. [172]

    Journal of Computational Physics , year = 1984, month = mar, volume =

    Adaptive Mesh Refinement for Hyperbolic Partial Differential Equations. Journal of Computational Physics , year = 1984, month = mar, volume =. doi:10.1016/0021-9991(84)90073-1 , adsurl =

    1984 doi

  165. [173]

    , year = 2024, month = jul, volume =

    Merging filaments II: The origin of the tuning fork. , year = 2024, month = jul, volume =. doi:10.1093/mnrasl/slae045 , adsurl =

    2024 doi

  166. [174]

    , keywords =

    Instability and Evolution of Shocked Clouds Formed by Orthogonal Collisions between Magnetized Filamentary Molecular Clouds. , keywords =. doi:10.3847/1538-4357/ad7389 , archivePrefix =. 2408.08863 , primaryClass =

    doi

  167. [175]

    Journal of Computational Physics , keywords =

    A low-dissipation HLLD approximate Riemann solver for a very wide range of Mach numbers. Journal of Computational Physics , keywords =. doi:10.1016/j.jcp.2021.110639 , archivePrefix =. 2108.04991 , primaryClass =

    2021 doi

  168. [176]

    , year = 1947, month = mar, volume =

    Small Dark Nebulae. , year = 1947, month = mar, volume =. doi:10.1086/144901 , adsurl =

    1947 doi

  169. [177]

    , keywords =

    Filament fragmentation: density gradients suppress end-dominated collapse. , keywords =. doi:10.1093/mnras/stad2517 , archivePrefix =. 2307.11162 , primaryClass =

    doi

  170. [178]

    , keywords =

    Gravitational collapse and fragmentation of isothermal, non-rotating, cylindrical clouds. , keywords =

  171. [179]

    , keywords =

    Gravitational fragmentation caught in the act: the filamentary Musca molecular cloud. , keywords =. doi:10.1051/0004-6361/201526017 , archivePrefix =. 1507.03742 , primaryClass =

    doi arXiv

  172. [180]

    , keywords =

    Isolating signatures of major cloud-cloud collisions using position-velocity diagrams. , keywords =. doi:10.1093/mnras/stv639 , archivePrefix =. 1503.06795 , primaryClass =

    doi arXiv

  173. [181]

    , keywords =

    Cloud-cloud collisions and triggered star formation. , keywords =. doi:10.1093/pasj/psaa103 , archivePrefix =. 2009.05077 , primaryClass =

    2009 doi

  174. [182]

    , keywords =

    Triggered O Star Formation in M20 via Cloud-Cloud Collision: Comparisons between High-resolution CO Observations and Simulations. , keywords =. doi:10.3847/1538-4357/835/2/142 , archivePrefix =. 1612.09458 , primaryClass =

    doi arXiv

  175. [183]

    , keywords =

    Evidence of Interacting Elongated Filaments in the Star-forming Site AFGL 5142. , keywords =. doi:10.3847/1538-4357/ab10dc , archivePrefix =. 1903.07099 , primaryClass =

    1903 doi arXiv

  176. [184]

    Protostars and Planets VII , year = 2023, editor =

    From Bubbles and Filaments to Cores and Disks: Gas Gathering and Growth of Structure Leading to the Formation of Stellar Systems. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2205.03935 , archivePrefix =. 2205.03935 , primaryClass =

    2023 doi

  177. [185]

    Annalen der Physik , year = 1834, month = jan, volume =

    Ueber die Figur des Gleichgewichts. Annalen der Physik , year = 1834, month = jan, volume =. doi:10.1002/andp.18341090808 , adsurl =

    doi

  178. [186]

    1988 , howpublished =

    Calculating the area and centroid of a polygon. 1988 , howpublished =

    1988

  179. [187]

    , keywords =

    Unveiling Physical Conditions and Star Formation Processes in the G47 Filamentary Cloud. , keywords =. doi:10.3847/1538-4357/adcee4 , archivePrefix =. 2504.04742 , primaryClass =

    doi

  180. [188]

    , keywords =

    IC 5146 Dark Streamer: The First Reliable Candidate of Edge Collapse, Hub-filament Systems, and Intertwined Sub-filaments. , keywords =. doi:10.3847/1538-4357/acbccc , archivePrefix =. 2302.07502 , primaryClass =

    doi

  181. [189]

    , keywords =

    Formation of the Hub-Filament System G33.92+0.11: Local Interplay between Gravity, Velocity, and Magnetic Field. , keywords =. doi:10.3847/1538-4357/abc74e , archivePrefix =. 2011.01555 , primaryClass =

    2011 doi

  182. [190]

    , keywords =

    G321.93-0.01: A Rare Site of Multiple Hub-filament Systems with Evidence of Collision and Merging of Filaments. , keywords =. doi:10.3847/1538-3881/ad98ff , archivePrefix =. 2411.13870 , primaryClass =

    doi

  183. [191]

    , keywords =

    Kinematics and Star Formation in the Hub Filament System G6.55-0.1. , keywords =. doi:10.3847/1538-4357/ad3df5 , archivePrefix =. 2404.07640 , primaryClass =

    doi

  184. [192]

    , keywords =

    Massive star formation in the hub-filament system of RCW 117. , keywords =. doi:10.1093/mnras/stad3385 , archivePrefix =. 2311.00477 , primaryClass =

    doi

  185. [193]

    , keywords =

    Observational Evidence of the Merging of Filaments and Hub Formation in G083.097+03.270. , keywords =. doi:10.3847/1538-4357/ad0048 , archivePrefix =. 2309.13912 , primaryClass =

    doi

  186. [194]

    The ALMA Survey of 70 m Dark High-mass Clumps in Early Stages (ASHES). IX. Physical Properties and Spatial Distribution of Cores in IRDCs. , keywords =. doi:10.3847/1538-4357/acccea , archivePrefix =. 2304.01757 , primaryClass =

    doi

  187. [195]

    On the clump mass concentration within the most massive cores

    An ALMA study of hub-filament systems - I. On the clump mass concentration within the most massive cores. , keywords =. doi:10.1093/mnras/stab2674 , archivePrefix =. 2109.07489 , primaryClass =

    doi

  188. [196]

    , keywords =

    Evidence of high-mass star formation through multiscale mass accretion in hub-filament-system clouds. , keywords =. doi:10.1093/mnras/stad047 , archivePrefix =. 2301.03144 , primaryClass =

    doi

  189. [197]

    From filaments to spheroids: the origin of the hub-filament systems

    Emergence of high-mass stars in complex fiber networks (EMERGE): V. From filaments to spheroids: the origin of the hub-filament systems. , keywords =. doi:10.1051/0004-6361/202450779 , archivePrefix =. 2411.05613 , primaryClass =

    doi

  190. [198]

    , keywords =

    New evidences in IRDC G333.73 + 0.37: colliding filamentary clouds, hub-filament system, and embedded cores. , keywords =. doi:10.1093/mnras/stac967 , archivePrefix =. 2204.02127 , primaryClass =

    doi

  191. [199]

    Multi-scale analysis of the Monoceros OB 1 star-forming region. II. Colliding filaments in the Monoceros OB1 molecular cloud. , keywords =. doi:10.1051/0004-6361/201834903 , archivePrefix =. 1909.06145 , primaryClass =

    1909 doi

  192. [200]

    , keywords =

    New Insights in the Mid-infrared Bubble N49 Site: A Clue of Collision of Filamentary Molecular Clouds. , keywords =. doi:10.3847/1538-4357/aa9be2 , archivePrefix =. 1711.06412 , primaryClass =

    doi arXiv

  193. [201]

    , keywords =

    Kinematic Structure of Molecular Gas around High-mass YSO, Papillon Nebula, in N159 East in the Large Magellanic Cloud: A New Perspective with ALMA. , keywords =. doi:10.3847/1538-4357/835/1/108 , archivePrefix =. 1604.06010 , primaryClass =

    doi arXiv

  194. [202]

    , keywords =

    Colliding Filaments and a Massive Dense Core in the Cygnus OB 7 Molecular Cloud. , keywords =. doi:10.1088/0004-637X/797/1/58 , archivePrefix =. 1411.0942 , primaryClass =

    doi arXiv

  195. [203]

    , keywords =

    Tracking Star-forming Cores as Mass Reservoirs in Clustered and Isolated Regions Using Numerical Passive Tracer Particles. , keywords =. doi:10.3847/1538-4357/ada602 , archivePrefix =. 2501.02225 , primaryClass =

    doi

  196. [204]

    , keywords =

    Filamentary Accretion Flows in the Embedded Serpens South Protocluster. , keywords =. doi:10.1088/0004-637X/766/2/115 , archivePrefix =. 1301.6792 , primaryClass =

    doi arXiv

  197. [205]

    , keywords =

    The Giant Molecular Cloud G148.24+00.41: gas properties, kinematics, and cluster formation at the nexus of filamentary flows. , keywords =. doi:10.1093/mnras/stae060 , archivePrefix =. 2401.03202 , primaryClass =

    doi

  198. [206]

    , keywords =

    New Insights into the H II Region G18.88-0.49: Hub-Filament System and Accreting Filaments. , keywords =. doi:10.3847/1538-4357/abb827 , archivePrefix =. 2009.05249 , primaryClass =

    2009 doi

  199. [207]

    , keywords =

    Near-Infrared Imaging Survey of Bok Globules: Density Structure. , keywords =. doi:10.1086/444619 , archivePrefix =. astro-ph/0506205 , primaryClass =

    doi arXiv

  200. [208]

    , keywords =

    Looking Into the Hearts of Bok Globules: Millimeter and Submillimeter Continuum Images of Isolated Star-forming Cores. , keywords =. doi:10.1088/0067-0049/188/1/139 , archivePrefix =. 1004.0869 , primaryClass =

    doi arXiv

  201. [209]

    , keywords =

    The role of molecular filaments in the origin of the prestellar core mass function and stellar initial mass function. , keywords =. doi:10.1051/0004-6361/201935915 , archivePrefix =. 1907.13448 , primaryClass =

    1907 doi

  202. [210]

    Journal of Computational Physics , year = 2010, month = mar, volume =

    Runge-Kutta methods with minimum storage implementations. Journal of Computational Physics , year = 2010, month = mar, volume =. doi:10.1016/j.jcp.2009.11.006 , adsurl =

    2010 doi

  203. [211]

    , keywords =

    Evolution of magnetized hub-filament systems: Comparing the observed properties of W3(OH), W3 Main, and S 106. , keywords =. doi:10.1051/0004-6361/202554901 , archivePrefix =. 2508.05918 , primaryClass =

    doi

  204. [212]

    , keywords =

    Gravitational collapse of the OMC-1 region. , keywords =. doi:10.1051/0004-6361/201730732 , archivePrefix =. 1703.03464 , primaryClass =

    doi arXiv

  205. [213]

    , keywords =

    Fibers in the NGC 1333 proto-cluster. , keywords =. doi:10.1051/0004-6361/201630348 , archivePrefix =. 1703.07029 , primaryClass =

    doi arXiv

  206. [214]

    , keywords =

    Direct Observational Evidence of the Multi-scale, Dynamical Mass Accretion Toward a High-mass Star-forming Hub-filament System. , keywords =. doi:10.3847/1538-4357/acdf42 , archivePrefix =. 2306.10332 , primaryClass =

    doi

  207. [215]

    , keywords =

    A quantification of the non-spherical geometry and accretion of collapsing cores. , keywords =. doi:10.1111/j.1365-2966.2010.17775.x , archivePrefix =. 1009.5395 , primaryClass =

    2010 doi

  208. [216]

    Subfilaments and velocities

    On the nature of star-forming filaments - II. Subfilaments and velocities. , keywords =. doi:10.1093/mnras/stv2559 , archivePrefix =. 1509.03321 , primaryClass =

    doi arXiv

  209. [217]

    , keywords =

    The CARMA-NRO Orion Survey: Filament Formation via Collision-induced Magnetic Reconnection the Stick in Orion A. , keywords =. doi:10.3847/1538-4357/abc687 , archivePrefix =. 2011.00183 , primaryClass =

    2011 doi

  210. [218]

    , keywords =

    Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation. , keywords =. doi:10.3847/1538-4357/ae12f4 , adsurl =

    doi

  211. [219]

    , keywords =

    Colliding filaments in the molecular cloud G34. , keywords =. doi:10.1051/0004-6361/202553851 , adsurl =

    doi

  212. [220]

    , keywords =

    Investigating the global collapse of filaments using smoothed particle hydrodynamics. , keywords =. doi:10.1093/mnras/stv393 , archivePrefix =. 1502.07552 , primaryClass =

    doi arXiv

  213. [221]

    , keywords =

    The Pipe Nebula as seen with Herschel: formation of filamentary structures by large-scale compression?. , keywords =. doi:10.1051/0004-6361/201118663 , archivePrefix =. 1203.3403 , primaryClass =

    doi arXiv

  214. [222]

    , keywords =

    The Herschel view of the dense core population in the Ophiuchus molecular cloud. , keywords =. doi:10.1051/0004-6361/201936442 , archivePrefix =. 2001.11036 , primaryClass =

    2001 doi

  215. [223]

    , keywords =

    A low-mass hub-filament with double centre revealed in NGC 2071-North. , keywords =. doi:10.1093/mnras/stad132 , archivePrefix =. 2301.00481 , primaryClass =

    doi

  216. [224]

    Growth of Massive Molecular Cloud Filament by Accretion Flows. II. New Mechanism to Support a Supercritical Filament Against Radial Collapse. , keywords =. doi:10.3847/1538-4357/add529 , archivePrefix =. 2410.04455 , primaryClass =

    doi

  217. [225]

    , keywords =

    Hub formation and filament-filament collision: An analytical model. , keywords =. doi:10.1093/pasj/psag036 , archivePrefix =. 2603.12876 , primaryClass =

    doi

Pith tools

Reviewed May 21, 2026 · model on record in the stance chip above.