pith. sign in

arxiv: 2605.20835 · v1 · pith:2KFJNLSWnew · submitted 2026-05-20 · 🌌 astro-ph.GA

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

Raiga Kashiwagi , Kazunari Iwasaki , Kohji Tomisaka , Tsuyoshi Inoue This is my paper

Pith reviewed 2026-05-21 03:52 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords filament collisionsoblique collisionsmagnetohydrodynamicsgravitational collapsemolecular cloudshub-filament systemsstar formation
0
0 comments X

The pith

Oblique collisions between magnetized filaments form compressed clouds whose collapse or expansion is set by the angle and an immediate energy balance check.

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

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.

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.

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.

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.

Where Pith is reading between the lines

These are 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.

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.

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.

Figures

Figures reproduced from arXiv: 2605.20835 by Kazunari Iwasaki, Kohji Tomisaka, Raiga Kashiwagi, Tsuyoshi Inoue.

Figure 1
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 … view at source ↗
Figure 2
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 th… view at source ↗
Figure 3
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… view at source ↗
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-dimensional density slices showing the evolution of the expansion mode for model L05V16th60. collapse to expansion when the other parameters… view at source ↗
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-dotted lines denote the collapse–expansion boundary, representing the threshold line mass (i.e., λ0/λcrit,B) at which the total energy of the co… view at source ↗
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, while the collision angle is varied from θ = π/2 to θ = 0. Star symbols show the mass of gas whose density exceeds the initial central densit… view at source ↗
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. For the dash-dotted lines, the geometric factor of the initial filament, η, is set to its average value for each β0: η = 0.65 for β0 = 1 and η… view at source ↗
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 schematic diagram on the x=0 plane showing the non-colliding filament segments. Vesc ≃ 1.5 cs–6 cs, indicating that the non-colliding segmen… view at source ↗
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.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

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

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.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 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.
axioms (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.

pith-pipeline@v0.9.0 · 5809 in / 1411 out tokens · 30805 ms · 2026-05-21T03:52:33.941217+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

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.

Reference graph

Works this paper leans on

225 extracted references · 225 canonical work pages · 96 internal anchors

  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 internal anchor Pith review Pith/arXiv 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 internal anchor Pith review Pith/arXiv 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 internal anchor Pith review Pith/arXiv 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 internal anchor Pith review Pith/arXiv 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

  9. [9]

    Quasi-periodic Fast Propagating Magnetoacoustic Waves during the Magnetic Reconnection Between Solar Coronal Loops

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aaf167 2018

  10. [10]

    Nominal values for selected solar and planetary quantities: IAU 2015 Resolution B3

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-6256/152/2/41 2015

  11. [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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/197/2/31 2011

  12. [12]

    Galaxy emission line classification using 3D line ratio diagrams

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/793/2/127 2014

  13. [13]

    Lemuridae , abstract =

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

    work page doi:10.1515/9781400880676-008

  14. [14]

    , year =

    Heard, Stephen B. , year =. Charles

    work page

  15. [15]

    Science Fiction Studies , author =

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

    work page 1979

  16. [16]

    Poetry , author =

    Lemur. Poetry , author =. 1996 , pages =

    work page 1996

  17. [17]

    , year =

    Wright, Patricia C. , year =. For the

    work page

  18. [18]

    McGoogan, Keriann , year =. Chasing

    work page

  19. [19]

    Magnetohydrostatic Equilibrium Structure and Mass of Filamentary Isothermal Cloud Threaded by Lateral Magnetic Field

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/785/1/24

  20. [20]

    Part III

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

    work page

  21. [21]

    Capozziello , V

    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 =

    work page doi:10.1111/j.1365-2966.2007.12750.x 2007

  22. [22]

    Polytropic models of filamentary interstellar clouds - I. Structure and stability

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2168

  23. [23]

    Characterizing interstellar filaments with Herschel in IC5146

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201116596

  24. [24]

    , keywords =

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

    work page doi:10.1093/pasj/50.6.577

  25. [25]

    Characterizing the properties of nearby molecular filaments observed with Herschel

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201832725

  26. [26]

    Herschel view of the Taurus B211/3 filament and striations: Evidence of filamentary growth?

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220500

  27. [27]

    , year = 1964, month = oct, volume =

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

    work page doi:10.1086/148005 1964

  28. [28]

    Near-Infrared Imaging Polarimetry Toward Serpens South: Revealing the Importance of the Magnetic Field

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/734/1/63

  29. [29]

    The Magnetic Field in Taurus Probed by Infrared Polarization

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/741/1/21

  30. [30]

    Polarization Structure of Filamentary Clouds

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/807/1/47

  31. [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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525896

  32. [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 =

    work page doi:10.3847/1538-4357/aba1e2 2007

  33. [33]

    From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014666

  34. [34]

    Herschel Space Observatory - 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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014759

  35. [35]

    Filamentary structures and compact objects in the Aquila and Polaris clouds observed by Herschel

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014668

  36. [36]

    A Herschel study of the properties of starless cores in the Polaris Flare dark cloud region using PACS and SPIRE

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014618

  37. [37]

    , keywords =

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

    work page doi:10.1086/162228

  38. [38]

    EVLA Observations of the Barnard 5 Star-Forming Core: Embedded Filaments Revealed

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/739/1/l2 2041

  39. [39]

    Initial conditions for star formation in clusters: physical and kinematical structure of the starless core Oph A-N6

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/745/2/117

  40. [40]

    , keywords =

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

    work page doi:10.1093/mnras/stz2234 1908

  41. [41]

    Dense core formation by fragmentation of velocity-coherent filaments in L1517

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201117039

  42. [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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425305

  43. [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 =

    work page doi:10.1093/mnras/staa3148 2009

  44. [44]

    , keywords =

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

    work page doi:10.3847/2041-8205/830/2/l23 2041

  45. [45]

    Relative Alignment Between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud using Low and High Density Tracers

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1eb0

  46. [46]

    On the relation between the column density structures and the magnetic field orientation in the Vela C molecular complex

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730608

  47. [47]

    , year = 1974, month = jul, volume =

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

    work page 1974

  48. [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 =

    work page doi:10.1093/mnras/145.3.271 1969

  49. [49]

    An introduction to the study of stellar structure

    work page

  50. [50]

    Polytropic models of filamentary interstellar clouds -II. Helical magnetic fields

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2194

  51. [51]

    From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.2458/azu_uapress_9780816531240-ch002 2014

  52. [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 =

    work page doi:10.3389/fspas.2019.00005 2019

  53. [53]

    , year = 1958, month = jan, volume =

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

    work page doi:10.1093/mnras/118.5.523 1958

  54. [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 =

    work page doi:10.1143/ptp.77.635 1987

  55. [55]

    , keywords =

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

    work page doi:10.1086/171162

  56. [56]

    MNRAS , keywords =

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

    work page doi:10.1046/j.1365-8711.2000.03066.x 2000

  57. [57]

    , keywords =

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

    work page doi:10.3847/1538-4365/ab929b 2005

  58. [58]

    , keywords =

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

    work page doi:10.1086/310975

  59. [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 =

    work page doi:10.1016/j.jcp.2005.02.017 2005

  60. [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 =

    work page doi:10.1007/s10915-008-9239-z 2009

  61. [61]

    Athena: A New Code for Astrophysical MHD

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/588755

  62. [62]

    , keywords =

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

    work page doi:10.1086/306249

  63. [63]

    Cluster Formation Triggered by Filament Collisions in Serpens South

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/791/2/l23 2041

  64. [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 =

    work page doi:10.1051/0004-6361/202038232 2008

  65. [65]

    Was a cloud-cloud collision the trigger of the recent star formation in Serpens?

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201015477

  66. [66]

    , keywords =

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

    work page doi:10.1093/mnras/stab1698

  67. [67]

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

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525861

  68. [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 =

    work page doi:10.1051/0004-6361/201834753 1910

  69. [69]

    , keywords =

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

    work page doi:10.1093/pasj/psz072 1906

  70. [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 =

    work page doi:10.1051/0004-6361/202038624 2012

  71. [71]

    , keywords =

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

    work page doi:10.1086/166684

  72. [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 =

    work page doi:10.1143/ptp.78.1273 1987

  73. [73]

    , year = 1978, month = jan, volume =

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

    work page 1978

  74. [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 =

    work page doi:10.3847/1538-4357/ab4189 1909

  75. [75]

    Formation of dense structures induced by filament collisions. 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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425234

  76. [76]

    Filamentary structure of star-forming complexes

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/700/2/1609 2005

  77. [77]

    The physical and dynamical structure of Serpens: 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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913919

  78. [78]

    , keywords =

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

    work page doi:10.1086/157936

  79. [79]

    Evolution of Angular Momentum Distribution during Star Formation

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/312417

  80. [80]

    Simulations of MHD Turbulence in a Strongly Magnetized Medium

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/324186

Showing first 80 references.