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REVIEW 3 major objections 6 minor 208 references

An ordered hourglass magnetic field around a massive protostar is dragged by rotation, outflow, and accretion, not by classic strong-field collapse.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-07-11 12:59 UTC pith:MYX6SEXT

load-bearing objection Clean ALMA hourglass that is perpendicular to the outflow/rotation axis; the morphology and kinematics already make the bulk-motion case without needing the DCF numbers. the 3 major comments →

arxiv 2607.04822 v1 pith:MYX6SEXT submitted 2026-07-06 astro-ph.GA

ALMA observations of Magnetic Fields in the Massive Star-forming Region IRAS 18360-0537

Shixian Mo , Keping Qiu , Qizhou Zhang , Junhao Liu , Josep Miquel Girart , Hauyu Baobab Liu , Zhi-Yun Li , Shanghuo Li
show 1 more author
Huei-Ru Vivien Chen
This is my paper
classification astro-ph.GA
keywords magnetic fieldshigh-mass star formationALMA polarizationhourglass morphologyoutflowcore rotationIRAS 18360-0537
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

High-mass star formation is still debated as either magnetically controlled or turbulence-dominated. This paper maps the magnetic field in IRAS 18360-0537 with ALMA polarized dust emission and finds a clear hourglass shape. The surprise is that the hourglass is oriented nearly perpendicular to both the outflow and the core rotation axis, and parallel to the core’s elongation—exactly the opposite of the classic magnetically regulated collapse picture. Velocity maps show the core is fast-rotating, the field edges follow the outflow cavity walls, and accretion flows run along the elongation. The authors conclude that bulk gas motions (rotation, outflow, accretion) have reshaped the field, so the ordered hourglass does not prove strong magnetic support at these scales. The result matters because it shows that an apparently textbook magnetic morphology can be a secondary product of the gas dynamics rather than the primary regulator of collapse.

Core claim

The clear hourglass-shaped magnetic field in IRAS 18360-0537 is nearly perpendicular to the outflow and rotation axes and aligned with the core elongation. This geometry, together with the measured rotation, outflow cavity coincidence, and accretion flows, shows that the field morphology is dominated by gas bulk motions rather than by classic magnetically regulated collapse at ~10^3–10^4 AU scales.

What carries the argument

ALMA 1.3 mm polarized dust emission that traces plane-of-sky magnetic-field orientation, combined with SiO and CH3OH kinematics that map the outflow, rotation, and accretion, and with energy ratios that compare magnetic, rotational, and outflow contributions.

Load-bearing premise

The Davis-Chandrasekhar-Fermi magnetic-field strength remains a usable upper-limit benchmark for energy comparisons even though the paper itself states that bulk motions invalidate the method’s core assumptions.

What would settle it

Higher-resolution polarization maps at a few hundred AU that recover a magnetic field aligned with the outflow/rotation axis, or direct Zeeman measurements showing a field much weaker than the 1.7 mG upper limit, would overturn the claim that bulk motions dominate.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Hourglass morphology alone cannot be taken as evidence of strong-field collapse without kinematic alignment checks.
  • Misaligned fields reduce magnetic braking efficiency, allowing larger disks and more fragmentation, matching the observed fast rotation and MM2 fragment.
  • Outflow cavity walls and accretion bridges can re-orient magnetic fields on envelope scales, so multi-scale polarization surveys must include velocity data.
  • DCF-derived field strengths in dynamically active cores should be treated strictly as upper limits when bulk motions are evident.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If bulk-motion reshaping is common, many published “hourglass = strong field” cases may need re-classification once full kinematics are available.
  • The same geometry could be searched for in other high-mass cores that already show misaligned outflows and ordered polarization.
  • Reduced braking from misalignment offers a natural route to the large rotationally supported structures needed for high-mass disk formation.

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

3 major / 6 minor

Summary. The paper presents ALMA Band 6 full-polarization continuum and spectral-line observations of the high-mass star-forming region IRAS 18360-0537. Polarized 1.3 mm dust emission reveals a clear hourglass-shaped magnetic field whose mean orientation is nearly perpendicular to the NE–SW outflow and core rotation axes and aligned with the NW–SE core elongation. Higher-resolution data show a more uniform field still aligned with the hourglass waist. SiO traces a bipolar outflow; CH3OH maps show a clear velocity gradient interpreted as fast rotation (and infall). Using DCF (with structure-function and model-fit angular dispersions, Q = 0.28) the authors adopt an upper-limit B_pos ≈ 1.7 mG and compare magnetic, rotational, and outflow energies, finding β_r-G ≈ 0.2–0.4 and outflow kinetic energy exceeding the magnetic energy. They conclude that the ordered hourglass is shaped by bulk gas motions (outflow cavity walls, rotation, accretion) rather than classic magnetically regulated collapse at ~10^3–10^4 AU scales, with possible implications for reduced magnetic braking and larger disks.

Significance. If the morphological and kinematic interpretation holds, the result is a clear counter-example to the common assumption that an ordered hourglass morphology at core scales signals strong-field, magnetically regulated collapse with field–outflow–rotation alignment. The multi-scale field orientation (ALMA C43-1/C43-4/5 plus SMA and BISTRO context), the cavity-wall coincidence, the high β_r-G relative to literature cores, and the centroid-velocity analysis of CH3OH together provide a concrete observational case that bulk motions can produce an apparently ordered hourglass while remaining misaligned with the angular-momentum axis. The work is part of a larger ALMA polarization survey and supplies a useful individual-source study for that sample. The morphological and kinematic evidence is self-supporting even if absolute DCF energetics remain uncertain.

major comments (3)
  1. Appendix A and §4.2: The authors correctly state that DCF assumptions (equipartition, turbulence-dominated distortions) are violated when bulk motions dominate the field morphology, yet still adopt B_pos,u = 1.7 mG (structure-function δφ = 9.2°, Q = 0.28) as the quantitative benchmark for outflow kinetic energy (8 imes10^45–4.3 imes10^46 erg) and β_r-B ≈ 0.3–0.4. Because residual bulk-motion contributions to both δφ and σ_turb are acknowledged but not fully removed, the absolute energy ranking language is overstated. The morphological misalignment, cavity-wall coincidence, high β_r-G, and centroid-velocity curves already support the bulk-motion claim without absolute B; the paper should either demote DCF to a strict upper-limit illustration or quantify how much larger the overestimate could be and rephrase the energy comparisons accordingly.
  2. §4.2 and Figure 6: The CH3OH centroid-velocity analysis yields enclosed masses of ~50 M☉ (blue lobe) and ~162 M☉ (red lobe) under a fixed-radius Keplerian-like assumption (R ~ 2500 AU). The large discrepancy is attributed to MM2 and asymmetry, yet both values are then used to support “strong rotational motion.” A clearer statement of which mass (or range) is adopted for the dynamical argument, and how inclination and non-Keplerian contributions affect the slope, is needed before the rotation-supported-disk interpretation can be taken as robust.
  3. §4.1–4.3: The claim that the initial field was already perpendicular to angular momentum (supported by private BISTRO communication) is load-bearing for the reduced-braking / larger-disk scenario. Without a published large-scale map or quantitative position-angle comparison, this remains an assertion. Either include the BISTRO position-angle statistics (or a figure) or clearly label the multi-scale alignment as preliminary and not required for the core-scale bulk-motion conclusion.
minor comments (6)
  1. Abstract and §1: “strong magnetic field strength estimated using the Davis-Chandrasekhar-Fermi method” should be qualified immediately as an upper limit, consistent with the later discussion.
  2. Figure 1(c) caption and text: SMA beam and rms are given; a brief note on why the hourglass is only recovered with ALMA (sensitivity vs. resolution) would help the reader.
  3. §2: The incorrect systemic-velocity configuration that nullified the FDM lines is mentioned; a short statement of the intended lines and the resulting loss of kinematic tracers would clarify the data limitations.
  4. Appendix A.2 / Figure 7: The CH3OH rotation-temperature map uses six transitions; listing the exact transitions and any optical-depth checks in the main text or table would improve reproducibility.
  5. Typos and notation: “condenstaion” (§4.1), inconsistent use of “MM1/MM2” vs. “condensations,” and occasional missing spaces around units (e.g., “1.7mG”). Standardize β_r-G / β_rot notation across text and Figure 5.
  6. Figure 4 lower panel: The schematic is helpful but the spiral/toroidal geometry is not quantitatively constrained; a short caveat that it is illustrative would avoid over-interpretation.

Circularity Check

1 steps flagged

No significant circularity: hourglass morphology, misalignment, and bulk-motion interpretation rest on new ALMA Stokes maps and independent kinematics; self-citations supply only prior masses/outflow parameters used as inputs.

specific steps
  1. self citation load bearing [§4.2 and Appendix A (mass, outflow energy, protostar mass inputs)]
    "we adopted the outflow mass of ∼54 M⊙ obtained by Qiu et al. (2012) from combined SMA and IRAM 30m CO data. ... our modeling in Mo & Qiu (2023) provides an alternative estimate of the infall velocity. ... The total gas mass is 80 M⊙ from the SMA observations (Qiu et al. 2012)"

    Secondary quantitative energy ratios (Eout, βr-B, βr-G, vinfall) rely on mass and kinematic parameters taken from prior papers by overlapping authors rather than re-derived solely from the present ALMA data. The dependence is not load-bearing for the primary morphological claim (misalignment + cavity-wall coincidence), which stands without those numbers; hence only a minor, non-central circularity.

full rationale

The paper is an observational study whose central claim (ordered hourglass B-field nearly perpendicular to outflow/rotation axes, therefore shaped by bulk motions rather than classic magnetically regulated collapse) is derived directly from the new ALMA Band-6 polarization maps (Figs. 1–2), SiO outflow morphology, and CH3OH velocity gradients (Fig. 3). These data products are independent of any fitted constant or self-defined quantity. Energetic comparisons in §4.2 adopt literature values (core mass ~80 M⊙, outflow mass, protostellar mass) from prior works by overlapping authors (Qiu et al. 2012; Mo & Qiu 2023) and treat the DCF Bpos,u = 1.7 mG explicitly as an upper limit after noting that DCF assumptions fail when bulk motions dominate (Appendix A). No equation reduces a claimed prediction to a fitted input by construction; no uniqueness theorem is imported; no ansatz is smuggled. The single minor self-citation chain supplies numerical inputs for secondary energy ratios but does not force the morphological conclusion. Score 1 reflects only that secondary dependence; the derivation chain itself is self-contained against the new observations.

Axiom & Free-Parameter Ledger

5 free parameters · 4 axioms · 0 invented entities

Central claim rests on standard dust-alignment and DCF machinery plus several numerical choices (Q factor, temperatures, masses, angular-dispersion method) that directly set the energy ratios used to argue bulk-motion dominance. No new physical entities are postulated; the interpretation re-uses existing MHD concepts of field dragging by rotation/outflow/accretion.

free parameters (5)
  • DCF correction factor Q = 0.28
    Adopted Q≈0.28 from Liu et al. (2022) clump/core simulations instead of the classical 0.5; directly scales B_pos and all subsequent energy ratios.
  • Angular dispersion δφ = 4.7° / 9.2°
    Two methods yield 4.7° (Ewertowski model) vs 9.2° (structure function); authors prefer the latter for the upper-limit B=1.7 mG used in energetics.
  • Dust/gas temperature bounds = 55–160 K
    NH3 kinetic T=55 K (lower) and CH3OH rotation T=160 K (upper) set mass and density ranges that enter B and β ratios.
  • Turbulent velocity after bulk-motion subtraction = 1.4 km s−1
    Reduced from observed 2.7 km s−1 linewidth to 1.4 km s−1 via RADMC-3D envelope-disk model (Mo & Qiu 2023); controls DCF B.
  • Outflow mass = 10–54 M⊙
    Two values used: 54 M⊙ (prior CO) and ~10 M⊙ (empirical M_out–M_clump scaling); both exceed magnetic energy.
axioms (4)
  • domain assumption Radiative Alignment Torque (RAT) theory: sub-100 µm grains align short axes with B, so polarized dust emission traces plane-of-sky B.
    Invoked throughout §1 and §3 to convert polarization position angles to B orientations; standard but untested at the highest densities here.
  • domain assumption Davis-Chandrasekhar-Fermi method equates turbulent kinetic and magnetic energies provided angular dispersion <25° and bulk motions are removed.
    Appendix A; authors note the assumption is likely violated yet still use the result as an upper limit.
  • domain assumption Observed NW-SE velocity gradient in CH3OH is dominated by rotation (with secondary infall contribution).
    §3.2, §4.2; used to compute β_r-B, β_r-G and to argue rotational dragging of field lines.
  • ad hoc to paper Parabolic / Ewertowski analytic models adequately subtract the large-scale ordered field for residual angular dispersion.
    Appendix A.1; choice of model changes δφ by factor ~2 and therefore B.

pith-pipeline@v1.1.0-grok45 · 34274 in / 3130 out tokens · 29123 ms · 2026-07-11T12:59:05.519755+00:00 · methodology

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read the original abstract

Assessing the significance of magnetic fields in high-mass star formation remains one of the most challenging topics in astrophysics. In this study, we present full polarization observations obtained from the Atacama Large Millimeter/Submillimeter Array (ALMA) of the high-mass star-forming region IRAS18360-0537. The polarized dust emission at 1.3 mm reveals a clear hourglass-shaped morphology of the magnetic field. Interestingly, the magnetic field orientation is nearly perpendicular to both the outflow and core rotation axes, while it aligns with the elongation of the core. This orientation poses challenges for interpretation, particularly in light of the strong magnetic field strength estimated using the Davis-Chandrasekhar-Fermi method. Several scenarios provide insights into the underlying reasons for this magnetic field morphology. A clear velocity gradient seen in high-density tracing of molecular spectral lines indicates that the core is fast-rotating. The curved outskirts of the magnetic fields coincide with the outflow cavity, suggesting a possible influence from the outflow. The accretion flows along the core's elongation are also notable. Our study shows that the morphology of the magnetic field is probably highly influenced by the gas bulk motions.

Figures

Figures reproduced from arXiv: 2607.04822 by Hauyu Baobab Liu, Huei-Ru Vivien Chen, Josep Miquel Girart, Junhao Liu, Keping Qiu, Qizhou Zhang, Shanghuo Li, Shixian Mo, Zhi-Yun Li.

Figure 1
Figure 1. Figure 1: (a) ALMA 1.3 mm dust continuum contours toward IRAS18360 overlaid polarization intensity maps (grayscale) and polarization orientations at lower resolution (∼1.2′′). The contour levels are -2, 3, 5, 7, 12, 20, 40, 90, 150, 260, 410 times the σ value of 1.3 mJy beam−1 . The polarization segments (drawn following the Nyquist sampling) are plotted above the 3σ level (σ = 95 µJy beam−1 ), with segment lengths … view at source ↗
Figure 2
Figure 2. Figure 2: Zoomed-in view of the blue rectangle area in [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: (a) The SiO (J=5-4) emission observed with the ALMA and integrated from 85.8 to 100.6 kms−1 for the blue-shifted lobe and from 106.0 to 120.8 kms−1 for the red-shifted lobe, shown in blue and red contours, respectively. The contour levels of SiO emission are 3, 5, 9, 17, 33, 65, 129, 257 times σ = 36 mJy beam−1 km s−1 . (b) The color image shows the first-moment map of the CH3OH (102,9 − 93,9) emission, an… view at source ↗
Figure 4
Figure 4. Figure 4: Upper Panel: The magnetic field lines (black segments) overplotted on the SiO (J=5-4) emissions (colored contours). The red and blue contours are the same as [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Ratio of rotational energy to gravitational energy βrot vs. core radius. Data for the sources shown are taken from Hull & Zhang (2019) and Pattle et al. (2021) except IRAS 18360 (this work). We have investigated those magnetic-detected sources as samples and ultimately selected those with the detection of velocity gradients or rotations, which are: L1448 IRS2 (Kwon et al. 2019), NGC1333 IRAS4A (Attard et a… view at source ↗
Figure 6
Figure 6. Figure 6: Top panel: Rotation curves for CH3OH(102,9 − 93,9) in IRAS 18360. The projected distance is calculated as the distance from the velocity centroid point to the best-fitted line passing through the maximum flux position of this transition. Bottom panel: The left and right plots show the best fits to the part of rotation curves for the blue-shifted lobe (below 103 km s−1 ) and the red-shifted lobe (above 104 … view at source ↗
Figure 7
Figure 7. Figure 7: The rotation temperature map for CH3OH. Only the locations with significant measurements in integrated flux (above 3σ) in all of the involved transitions are included in the map. The continuum contours adopt the same levels as [PITH_FULL_IMAGE:figures/full_fig_p017_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Top panel: Contour map of the total (Stokes I) dust emission and the magnetic field vectors (The black contours are same as [PITH_FULL_IMAGE:figures/full_fig_p020_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Structure function for a center region of IRAS 18360. The measured angle dispersion is shown in black solid circles with the error bars. The best is shown by the blue dashed line. The vertical dashed line represents the beam size of the observations ∼ 1.1 ′′ and the horizontal red dashed line is the predicted angle dispersion for a random field ∼ 52◦ . Ballesteros-Paredes, J., Klessen, R. S., & V´azquez-Se… view at source ↗
Figure 10
Figure 10. Figure 10: Spatial distribution of the B-field-to-gravity force ratio ΣB toward IRAS18360. The contour levels are the same as in [PITH_FULL_IMAGE:figures/full_fig_p022_10.png] view at source ↗

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Works this paper leans on

208 extracted references · 114 canonical work pages · 104 internal anchors

  1. [1]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1086/346149

  2. [2]

    Massive star formation via high accretion rates and early disk-driven outflows

    Massive Star Formation via High Accretion Rates and Early Disk-driven Outflows. , keywords =. doi:10.1086/512010 , archivePrefix =. astro-ph/0612674 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/512010

  3. [3]

    , keywords =

    Star formation through gravitational collapse and competitive accretion. , keywords =. doi:10.1111/j.1365-2966.2006.10495.x , archivePrefix =. astro-ph/0604615 , primaryClass =

    doi:10.1111/j.1365-2966.2006.10495.x 2006

  4. [4]

    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 =

    Pith/arXiv arXiv doi:10.2458/azu_uapress_9780816531240-ch002 2014

  5. [5]

    Magnetohydronamic Evolution of HII Regions in Molecular Clouds: Simulation Methodology, Tests, and Uniform Media

    Magnetohydrodynamic Evolution of H II Regions in Molecular Clouds: Simulation Methodology, Tests, and Uniform Media. , keywords =. doi:10.1086/522665 , archivePrefix =. astro-ph/0606539 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/522665

  6. [6]

    Infall-Driven Protostellar Accretion and the Solution to the Luminosity Problem

    Infall-driven Protostellar Accretion and the Solution to the Luminosity Problem. , keywords =. doi:10.1088/0004-637X/797/1/32 , archivePrefix =. 1407.1445 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/797/1/32

  7. [7]

    Collapse of Magnetized Molecular Cloud Cores. I. Semianalytical Solution. , keywords =. doi:10.1086/173305 , adsurl =

    work page doi:10.1086/173305

  8. [8]

    Collapse of Magnetized Molecular Cloud Cores. II. Numerical Results. , keywords =. doi:10.1086/173306 , adsurl =

    work page doi:10.1086/173306

  9. [9]

    Collapse of Magnetized Singular Isothermal Toroids. II. Rotation and Magnetic Braking. , keywords =. doi:10.1086/379243 , archivePrefix =. astro-ph/0311377 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/379243

  10. [10]

    Testing Magnetic Star Formation Theory

    Testing Magnetic Star Formation Theory. , keywords =. doi:10.1088/0004-637X/692/1/844 , archivePrefix =. 0807.2862 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/692/1/844

  11. [11]

    , keywords =

    Dissipation in Compressible Magnetohydrodynamic Turbulence. , keywords =. doi:10.1086/311718 , archivePrefix =. astro-ph/9809357 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/311718

  12. [12]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1086/307956

  13. [13]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1086/320636

  14. [14]

    , keywords =

    Star formation in molecular clouds: observation and theory. , keywords =. doi:10.1146/annurev.aa.25.090187.000323 , adsurl =

    doi:10.1146/annurev.aa.25.090187.000323

  15. [15]

    Magnetic Braking, Ambipolar Diffusion, and the Formation of Cloud Cores and Protostars. I. Axisymmetric Solutions. , keywords =. doi:10.1086/174611 , adsurl =

    doi:10.1086/174611

  16. [16]

    , keywords =

    Observational Constraints on the Ages of Molecular Clouds and the Star Formation Timescale: Ambipolar-Diffusion-controlled or Turbulence-induced Star Formation?. , keywords =. doi:10.1086/500125 , archivePrefix =. astro-ph/0512043 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/500125

  17. [17]

    Science , keywords =

    Magnetic Fields in the Formation of Massive Stars. Science , keywords =. doi:10.1126/science.1171807 , adsurl =

    work page doi:10.1126/science.1171807

  18. [18]

    , keywords =

    Submillimeter Array Observations of Magnetic Fields in G240.31+0.07: An Hourglass in a Massive Cluster-forming Core. , keywords =. doi:10.1088/2041-8205/794/1/L18 , archivePrefix =. 1409.5608 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/2041-8205/794/1/l18 2041

  19. [19]

    Evolution of Magnetic Fields in High Mass Star Formation: Linking field geometry and collapse for the W51 e2/e8 cores

    Evolution of Magnetic Fields in High-Mass Star Formation: Linking Field Geometry and Collapse for the W51 e2/e8 Cores. , keywords =. doi:10.1088/0004-637X/700/1/251 , archivePrefix =. 0905.1996 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/700/1/251 1996

  20. [20]

    High Resolution Millimeter-Wave Mapping of Linearly Polarized Dust Emission: Magnetic Field Structure in Orion

    High-Resolution Millimeter-Wave Mapping of Linearly Polarized Dust Emission: Magnetic Field Structure in Orion. , keywords =. doi:10.1086/311485 , archivePrefix =. astro-ph/9805288 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/311485

  21. [21]

    Magnetic field structure in a high-mass outflow/disk system

    Magnetic Field Structure in a High-mass Outflow/Disk System. , keywords =. doi:10.1088/2041-8205/724/1/L113 , archivePrefix =. 1010.3635 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/724/1/l113 2041

  22. [22]

    , keywords =

    Polarization Properties and Magnetic Field Structures in the High-mass Star-forming Region W51 Observed with ALMA. , keywords =. doi:10.3847/1538-4357/aaa4c1 , archivePrefix =. 1801.08264 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aaa4c1

  23. [23]

    Frontiers in Astronomy and Space Sciences , keywords =

    Interferometric observations of magnetic fields in forming stars. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2019.00003 , archivePrefix =. 1903.03177 , primaryClass =

    doi:10.3389/fspas.2019.00003 2019

  24. [24]

    Comparing star formation models with interferometric observations of the protostar NGC 1333 IRAS 4A. I. Magnetohydrodynamic collapse models. , keywords =. doi:10.1051/0004-6361/201117813 , archivePrefix =. 1109.6251 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201117813

  25. [25]

    Forming an O Star via Disk Accretion?

    Forming an O Star via Disk Accretion?. , keywords =. doi:10.1088/0004-637X/756/2/170 , archivePrefix =. 1207.4817 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/756/2/170

  26. [26]

    Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

    CASA Architecture and Applications. Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

    2007

  27. [27]

    , 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 =

    Pith/arXiv arXiv doi:10.1088/0004-637x/790/2/84

  28. [28]

    Science , keywords =

    Magnetic Fields in the Formation of Sun-Like Stars. Science , keywords =. doi:10.1126/science.1129093 , archivePrefix =. astro-ph/0609177 , primaryClass =

    Pith/arXiv arXiv doi:10.1126/science.1129093

  29. [29]

    IRAS 16293: A "Magnetic" Tale of Two Cores

    IRAS 16293: A ``Magnetic'' Tale of Two Cores. , keywords =. doi:10.1088/0004-637X/707/2/921 , archivePrefix =. 0910.5269 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/707/2/921

  30. [30]

    , keywords =

    TADPOL: A 1.3 mm Survey of Dust Polarization in Star-forming Cores and Regions. , keywords =. doi:10.1088/0067-0049/213/1/13 , archivePrefix =. 1310.6653 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0067-0049/213/1/13

  31. [31]

    Dust Polarization toward Embedded Protostars in Ophiuchus with ALMA. II. IRAS 16293-2422. , keywords =. doi:10.3847/1538-4357/aaef81 , archivePrefix =. 1811.03104 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaef81

  32. [32]

    Dust Polarization toward Embedded Protostars in Ophiuchus with ALMA. I. VLA 1623. , keywords =. doi:10.3847/1538-4357/aac21a , archivePrefix =. 1804.05968 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aac21a

  33. [33]

    , keywords =

    Magnetic Braking, Ambipolar Diffusion, Cloud Cores, and Star Formation: Natural Length Scales and Protostellar Masses. , keywords =. doi:10.1086/170035 , adsurl =

    work page doi:10.1086/170035

  34. [34]

    , keywords =

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

    doi:10.1086/154835

  35. [35]

    Nonhomologous contraction and equilibria of self-gravitating, magnetic interstellar clouds embedded in an intercloud medium: star formation. I. Formulation of the problem and method of solution. , keywords =. doi:10.1086/154436 , adsurl =

    doi:10.1086/154436

  36. [36]

    Nonhomologous contraction and equilibria of self-gravitating, magnetic interstellar clouds embedded in an intercloud medium: star formation. II. Results. , keywords =. doi:10.1086/154478 , adsurl =

    doi:10.1086/154478

  37. [37]

    , year = 1985, month = nov, volume =

    The Angular Momentum Problem during Star Formation - Magnetically Linked Aligned Rotators - Part Two - Results. , year = 1985, month = nov, volume =. doi:10.1086/163599 , adsurl =

    work page doi:10.1086/163599 1985

  38. [38]

    The Magnetic Field Morphology of the Class 0 Protostar L1157-mm

    The Magnetic Field Morphology of the Class 0 Protostar L1157-mm. , keywords =. doi:10.1088/2041-8205/769/1/L15 , archivePrefix =. 1304.6739 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/769/1/l15 2041

  39. [39]

    , keywords =

    A Mathematical Model for an Hourglass Magnetic Field. , keywords =. doi:10.1088/0004-637X/767/1/33 , archivePrefix =. 1302.6913 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/767/1/33

  40. [40]

    , keywords =

    Studies of Regular and Random Magnetic Fields in the ISM: Statistics of Polarization Vectors and the Chandrasekhar-Fermi Technique. , keywords =. doi:10.1086/587479 , archivePrefix =. 0801.0279 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/587479

  41. [41]

    Dispersion of Magnetic Fields in Molecular Clouds. I. , keywords =. doi:10.1088/0004-637X/696/1/567 , archivePrefix =. 0811.0813 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/696/1/567

  42. [42]

    , year = 1951, month = sep, volume =

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

    doi:10.1086/145464 1951

  43. [43]

    , year = 1953, month = jul, volume =

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

    doi:10.1086/145731 1953

  44. [44]

    , keywords =

    SCUBA Polarization Measurements of the Magnetic Field Strengths in the L183, L1544, and L43 Prestellar Cores. , keywords =. doi:10.1086/379705 , archivePrefix =. astro-ph/0305604 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/379705

  45. [45]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1093/mnras/stt561

  46. [46]

    , keywords =

    Population Diagram Analysis of Molecular Line Emission. , keywords =. doi:10.1086/307195 , adsurl =

    doi:10.1086/307195

  47. [47]

    , keywords =

    Turbulence and star formation in molecular clouds. , keywords =. doi:10.1093/mnras/194.4.809 , adsurl =

    doi:10.1093/mnras/194.4.809

  48. [48]

    Turbulence in the Interstellar Medium

    Turbulence in the interstellar medium. Nonlinear Processes in Geophysics , keywords =. doi:10.5194/npg-21-587-2014 , archivePrefix =. 1404.3691 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.5194/npg-21-587-2014 2014

  49. [49]

    Magnetically Dominated Parallel Interstellar Filaments at the Infrared Dark Cloud G14.225-0.506

    Magnetically Dominated Parallel Interstellar Filaments in the Infrared Dark Cloud G14.225-0.506. , keywords =. doi:10.3847/0004-637X/832/2/186 , archivePrefix =. 1609.08052 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/832/2/186

  50. [50]

    Multi-scale Dust Polarization and Spiral-like Stokes-I Residual in the Class I Protostellar System TMC-1A

    Multi-scale Dust Polarization and Spiral-like Stokes-I Residual in the Class I Protostellar System TMC-1A. , keywords =. doi:10.3847/1538-4357/ac15f3 , archivePrefix =. 2107.10646 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac15f3

  51. [51]

    Resolution-dependent Subsonic Non-thermal Line Dispersion Revealed by ALMA

    Resolution-dependent subsonic non-thermal line dispersion revealed by ALMA. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/21/1/24 , archivePrefix =. 2006.04168 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1674-4527/21/1/24 2006

  52. [52]

    Universe , keywords =

    Exploring the Spectral Line Broadening of the Bulk Motions in the High Mass Star Forming Region with Radiative Transfer Simulations. Universe , keywords =. doi:10.3390/universe9090415 , adsurl =

    work page doi:10.3390/universe9090415

  53. [53]

    , year = 1978, month = jan, volume =

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

    1978

  54. [54]

    Fragmentation at the Earliest Phase of Massive Star Formation

    Fragmentation at the Earliest Phase of Massive Star Formation. , keywords =. doi:10.1088/0004-637X/696/1/268 , archivePrefix =. 0902.0647 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/696/1/268

  55. [55]

    , year = 1956, month = jan, volume =

    Star formation in magnetic dust clouds. , year = 1956, month = jan, volume =. doi:10.1093/mnras/116.5.503 , adsurl =

    doi:10.1093/mnras/116.5.503 1956

  56. [56]

    The Origin of Stars and Planetary Systems , year = 1999, editor =

    Magnetic Fields and Star Formation: A Theory Reaching Adulthood. The Origin of Stars and Planetary Systems , year = 1999, editor =

    1999

  57. [57]

    Second Core Formation and High Speed Jets: Resistive MHD Nested Grid Simulations

    Second Core Formation and High-Speed Jets: Resistive Magnetohydrodynamic Nested Grid Simulations. , keywords =. doi:10.1086/507179 , archivePrefix =. astro-ph/0603456 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/507179

  58. [58]

    , keywords =

    Theory of Star Formation. , keywords =. doi:10.1146/annurev.astro.45.051806.110602 , archivePrefix =. 0707.3514 , primaryClass =

    Pith/arXiv arXiv doi:10.1146/annurev.astro.45.051806.110602

  59. [59]

    , keywords =

    Density, Velocity, and Magnetic Field Structure in Turbulent Molecular Cloud Models. , keywords =. doi:10.1086/318290 , archivePrefix =. astro-ph/0008454 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/318290

  60. [60]

    Dispersion of Magnetic Fields in Molecular Clouds. II. , keywords =. doi:10.1088/0004-637X/706/2/1504 , archivePrefix =. 0909.5227 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/706/2/1504

  61. [61]

    Dispersion of Magnetic Fields in Molecular Clouds. IV. Analysis of Interferometry Data. , keywords =. doi:10.3847/0004-637X/820/1/38 , archivePrefix =. 1602.01873 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/0004-637x/820/1/38

  62. [62]

    A generalized outflow criterion

    Magnetic fields during the early stages of massive star formation - II. A generalized outflow criterion. , keywords =. doi:10.1111/j.1365-2966.2012.20610.x , archivePrefix =. 1109.4379 , primaryClass =

    doi:10.1111/j.1365-2966.2012.20610.x 2012

  63. [63]

    Gravity and rotation drag the magnetic field in high-mass star formation

    Gravity and Rotation Drag the Magnetic Field in High-mass Star Formation. , keywords =. doi:10.3847/1538-4357/abc019 , archivePrefix =. 2010.05825 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/abc019 2010

  64. [64]

    Gravity Driven Magnetic Field at ~1000 au Scales in High-mass Star Formation

    Gravity-driven Magnetic Field at 1000 au Scales in High-mass Star Formation. , keywords =. doi:10.3847/2041-8213/ac081c , archivePrefix =. 2106.03866 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ac081c 2041

  65. [65]

    ALMA observations of dust polarization and molecular line emission from the Class 0 protostellar source Serpens SMM1

    ALMA Observations of Dust Polarization and Molecular Line Emission from the Class 0 Protostellar Source Serpens SMM1. , keywords =. doi:10.3847/1538-4357/aa7fe9 , archivePrefix =. 1707.03827 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa7fe9

  66. [66]

    OMC-1 dust polarisation in ALMA Band 7: Diagnosing grain alignment mechanisms in the vicinity of Orion Source I

    OMC-1 dust polarization in ALMA Band 7: diagnosing grain alignment mechanisms in the vicinity of Orion Source I. , keywords =. doi:10.1093/mnras/stab608 , archivePrefix =. 2009.14758 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab608 2009

  67. [67]

    Magnetic Field Structure in Spheroidal Star-forming Clouds. II. Estimating Field Structure from Observed Maps. , keywords =. doi:10.3847/1538-4357/ab9110 , archivePrefix =. 2005.04307 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab9110 2005

  68. [68]

    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 =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201425305

  69. [69]

    , 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 =

    Pith/arXiv arXiv doi:10.1086/587166

  70. [70]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1088/0004-637x/741/1/21

  71. [71]

    , 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 =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201220500

  72. [72]

    Tracing the magnetic field morphology of the Lupus I molecular cloud

    Tracing the Magnetic Field Morphology of the Lupus I Molecular Cloud. , keywords =. doi:10.1088/0004-637X/807/1/5 , archivePrefix =. 1504.08222 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/807/1/5

  73. [73]

    , keywords =

    The magnetic field and dust filaments in the Polaris Flare. , keywords =. doi:10.1093/mnras/stw1678 , archivePrefix =. 1607.00005 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw1678

  74. [74]

    Magnetic Fields and Massive Star Formation

    Magnetic Fields and Massive Star Formation. , keywords =. doi:10.1088/0004-637X/792/2/116 , archivePrefix =. 1407.3984 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/792/2/116

  75. [75]

    A Pseudodisk Threaded with a Toroidal and Pinched Poloidal Magnetic Field Morphology in the HH 211 Protostellar System

    A Pseudodisk Threaded with a Toroidal and Pinched Poloidal Magnetic Field Morphology in the HH 211 Protostellar System. , keywords =. doi:10.3847/1538-4357/ab2458 , archivePrefix =. 1905.09417 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab2458 1905

  76. [76]

    SMA observations of the polarized dust emission in solar-type Class 0 protostars: the magnetic field properties at envelope scales

    SMA observations of polarized dust emission in solar-type Class 0 protostars: Magnetic field properties at envelope scales. , keywords =. doi:10.1051/0004-6361/201833004 , archivePrefix =. 1804.05801 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833004

  77. [77]

    An observational correlation between magnetic field, angular momentum and fragmentation in the envelopes of Class 0 protostars?

    An observational correlation between magnetic field, angular momentum and fragmentation in the envelopes of Class 0 protostars?. , keywords =. doi:10.1051/0004-6361/202038854 , archivePrefix =. 2010.12466 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202038854 2010

  78. [78]

    The JCMT BISTRO survey: alignment between outflows and magnetic fields in dense cores/clumps

    The JCMT BISTRO Survey: Alignment between Outflows and Magnetic Fields in Dense Cores/Clumps. , keywords =. doi:10.3847/1538-4357/abca99 , archivePrefix =. 2011.06731 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/abca99 2011

  79. [79]

    Magnetically regulated disk-formation in the inner 100 au region of the Class 0 young stellar object OMC-3/MMS~6 resolved by JVLA and ALMA

    Magnetically Regulated Disk Formation in the Inner 100 au Region of the Class 0 Young Stellar Object OMC-3/MMS 6 Resolved by JVLA and ALMA. , keywords =. doi:10.3847/1538-4357/abf8b6 , archivePrefix =. 2010.05392 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/abf8b6 2010

  80. [80]

    Magnetic fields in star-forming systems (II): examining dust polarization, the Zeeman effect, and the Faraday rotation measure as magnetic field tracers

    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 internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa3148 2009

Showing first 80 references.