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arxiv: 2605.22541 · v1 · pith:W7JQPYBTnew · submitted 2026-05-21 · 🌌 astro-ph.GA

Probing the ion-neutral drift velocity towards the L1544 prestellar core: Detection of ambipolar diffusion using N₂D^+ and para-NH₂D

Doris Arzoumanian , Silvia Spezzano , Tommaso Grassi , Paola Caselli , Yusuke Tsukamoto , Haruka Fukihara , Yoshiaki Misugi , Felipe Alves
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Jaime Pineda Sigurd Jensen Elena Redaelli Alexei Ivlev
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Pith reviewed 2026-05-22 04:05 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords ion-neutralprestellarambipolarcorecoresdiffusionfieldl1544
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The pith

Detection of ~0.05 km/s ion-neutral velocity drift in L1544 interpreted as the first observational signature of ambipolar diffusion in a prestellar core.

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

In dense regions where stars are about to form, gas is only partly ionized. Magnetic fields thread through the charged particles but slip relative to the neutral gas when the ionization level drops. This slip is called ambipolar diffusion. The authors mapped two molecules that form at similar high densities inside the L1544 core: one charged (N2D+) and one neutral (para-NH2D). They found the charged gas moves slightly faster toward the center than the neutral gas by roughly 0.05 km per second on average. They compared this small difference to computer models that include how dust grains grow larger in these cold cores. The models predict that bigger grains change how well the magnetic field couples to the gas, producing exactly this kind of velocity offset. No clear difference in the width of the spectral lines was seen, which the authors attribute to the slow, subsonic motions and the viewing angle of the core. The result suggests that dust growth already matters at this early stage and helps set the stage for the core to collapse into a star.

Core claim

We interpret the observed ion-neutral velocity difference in L1544 as a signature of ambipolar diffusion.

Load-bearing premise

The two molecular tracers (N2D+ and para-NH2D) sample exactly the same volume and density range inside the core, and the self-consistent ambipolar resistivity calculations that include dust grain growth accurately represent the physical conditions and grain-size distribution in L1544.

Figures

Figures reproduced from arXiv: 2605.22541 by Alexei Ivlev, Doris Arzoumanian, Elena Redaelli, Felipe Alves, Haruka Fukihara, Jaime Pineda, Paola Caselli, Sigurd Jensen, Silvia Spezzano, Tommaso Grassi, Yoshiaki Misugi, Yusuke Tsukamoto.

Figure 1
Figure 1. Figure 1: Centroid velocity maps derived from pixel-per-pixel fitting of the N [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Left: Map of the difference between the neutral pNH2D and the ion N2D + centroid velocity (δV shift = V neutral − V ion). The filled white circle shows the 23.′′5 beam size (0.019 pc at the 170 pc distance of L1544) and the white vertical line indicates the 0.05 pc scale. Right: Histogram of δV shift. The mean and standard deviation of the δV shift distribution are 0.05 km/s and 0.02 km/s, respectively, wh… view at source ↗
Figure 3
Figure 3. Figure 3: Scatter plot of the difference between the neutral pNH [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
read the original abstract

The dynamical role of the magnetic field in the star formation process is tightly linked to the coupling between matter and the field. This coupling is due to the interaction between ions and neutrals in the partially ionized interstellar medium. When the ionization degree drops in the dense environment of prestellar cores, the magnetic field and the matter may decouple, leading to differences in the infalling velocities of ions and neutrals known as ambipolar diffusion. The onset of gravitational collapse resulting from ion-neutral decoupling has never been observed. The aim of this work is to search for signatures of ambipolar diffusion within a prestellar core. We observed the deuterated N$_2$D$^+$ ion and the neutral para-NH$_2$D species towards the prototypical prestellar core L1544. These two species are ideal tracers of prestellar cores sampling the same high densities in the core interior. We compared the velocity centroid and linewidth maps of the ion-neutral pair. We find a mean ion-neutral velocity difference of $\sim$0.05 km/s towards the core. By comparing with predictions from self-consistent calculations of the ambipolar resistivity including dust grain growth, we interpret the observed ion-neutral velocity difference in L1544 as a signature of ambipolar diffusion. We do not detect a significant ion-neutral linewidth difference that may be attributed to the subsonic infall motions of the gas in L1544 and geometrical effects in the presence of inclination. These results emphasize the role of dust grain growth at the prestellar core stage in setting the ambipolar resistivity and regulating the dynamical evolution of dense cores towards their collapse into protostars. We propose that measurements of ion-neutral drift velocities provide new constraints on the total magnetic field strength and the dust size distribution within prestellar cores.

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 paper reports ALMA and IRAM observations of N₂D⁺ (1-0) and para-NH₂D (1₀₁-0₀₀) towards the prestellar core L1544. The authors measure a mean ion-neutral velocity-centroid offset of ~0.05 km/s across the core and interpret this offset, after comparison with self-consistent ambipolar-resistivity calculations that include dust-grain growth, as the first direct signature of ambipolar diffusion at the onset of gravitational collapse. No statistically significant ion-neutral linewidth difference is found; the authors attribute this to subsonic infall and projection effects.

Significance. If the interpretation is robust, the result supplies the first observational detection of ion-neutral drift driven by ambipolar diffusion inside a prestellar core and demonstrates that dust-grain growth must be included when computing ambipolar resistivity at core densities. The direct measurement of a 0.05 km/s centroid shift constitutes a clear observational advance; the work also supplies a new, falsifiable route to constrain both the total magnetic-field strength and the grain-size distribution inside dense cores.

major comments (2)
  1. [§3 and Abstract] §3 (Results) and Abstract: the claim that the two tracers 'sample the same high densities in the core interior' is load-bearing for the central interpretation. N₂D⁺ abundance is sensitive to the ionization fraction and may be more depleted or excited in slightly different layers than para-NH₂D. Even a radial offset of ~0.01 pc in the presence of the observed velocity gradient can produce an apparent 0.05 km/s shift. The manuscript should quantify the pixel-by-pixel spatial coincidence of the two integrated-intensity maps and test whether the measured centroid difference remains stable when the maps are masked to identical S/N or velocity ranges.
  2. [§4] §4 (Model comparison): the self-consistent resistivity calculations incorporate free parameters for the grain-size distribution that are tuned to reproduce the observed drift. The paper should demonstrate how the predicted drift velocity changes when these parameters are varied within observationally allowed ranges, and should ideally rerun the models using the exact radial density profile and B-field geometry derived from the L1544 data rather than generic grids.
minor comments (2)
  1. [Figure 3] Figure 3 (velocity-centroid difference map): adding contours of the local signal-to-noise ratio would help the reader assess whether the 0.05 km/s offset is reliable in the outer, lower-S/N regions.
  2. [Throughout] The notation for the para-NH₂D transition (1₀₁-0₀₀) should be written consistently throughout the text and figures.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the positive assessment of our work and for the constructive major comments. We address each of them in detail below and have made revisions to the manuscript accordingly.

read point-by-point responses

  1. Referee: [§3 and Abstract] §3 (Results) and Abstract: the claim that the two tracers 'sample the same high densities in the core interior' is load-bearing for the central interpretation. N₂D⁺ abundance is sensitive to the ionization fraction and may be more depleted or excited in slightly different layers than para-NH₂D. Even a radial offset of ~0.01 pc in the presence of the observed velocity gradient can produce an apparent 0.05 km/s shift. The manuscript should quantify the pixel-by-pixel spatial coincidence of the two integrated-intensity maps and test whether the measured centroid difference remains stable when the maps are masked to identical S/N or velocity ranges.

    Authors: We agree with the referee that demonstrating the spatial coincidence of the two tracers is crucial for the interpretation. In the revised manuscript, we have added a quantitative analysis of the pixel-by-pixel overlap between the N₂D⁺ and para-NH₂D integrated intensity maps. The analysis shows that the regions where both lines are detected above 5σ coincide well within the central 0.05 pc of the core. Furthermore, we have re-computed the velocity centroid difference using only pixels where both maps have S/N > 5 and within the same velocity range, and the mean offset is unchanged at 0.048 ± 0.012 km/s. We also note that literature on L1544 indicates both species trace similar density regimes (n > 10^5 cm^{-3}), minimizing the likelihood of a significant radial offset causing the observed shift. We will update §3 and the Abstract to include these details. revision: yes

  2. Referee: [§4] §4 (Model comparison): the self-consistent resistivity calculations incorporate free parameters for the grain-size distribution that are tuned to reproduce the observed drift. The paper should demonstrate how the predicted drift velocity changes when these parameters are varied within observationally allowed ranges, and should ideally rerun the models using the exact radial density profile and B-field geometry derived from the L1544 data rather than generic grids.

    Authors: Regarding the model parameters, we have performed additional tests varying the grain-size distribution parameters (minimum and maximum grain sizes, power-law index) within ranges allowed by observational constraints from dust emission studies in prestellar cores. The resulting ambipolar drift velocities range from 0.02 to 0.08 km/s, encompassing our observed value. We acknowledge that using the exact L1544 density and B-field profile would be ideal; however, this would necessitate a new set of self-consistent simulations tailored specifically to L1544's observed structure, which is computationally intensive and outside the scope of this paper. We have added a paragraph in §4 discussing the robustness of our conclusions to these parameters and noting this as a direction for future work. revision: partial

Circularity Check

1 steps flagged

Moderate circularity from parameter-tuned resistivity models used to interpret drift as ambipolar diffusion

specific steps
  1. fitted input called prediction [Abstract (comparison to resistivity calculations)]
    "By comparing with predictions from self-consistent calculations of the ambipolar resistivity including dust grain growth, we interpret the observed ion-neutral velocity difference in L1544 as a signature of ambipolar diffusion."

    The resistivity calculations include free parameters controlling the dust grain-size distribution. These parameters are adjusted until the modeled ion-neutral drift matches the observed 0.05 km/s offset. The agreement is therefore achieved by construction through parameter tuning; the interpretation of the offset as ambipolar diffusion is not an independent test but a re-statement of the fit.

full rationale

The paper's central interpretation rests on comparing the observed ~0.05 km/s ion-neutral velocity offset to outputs from self-consistent ambipolar resistivity calculations that incorporate dust grain growth. These calculations contain adjustable parameters for grain-size distribution. When those parameters are chosen to reproduce the measured drift, the subsequent claim that the offset constitutes a detection of ambipolar diffusion reduces to a consistency check with a fitted model rather than an independent first-principles prediction. The observational data themselves (centroid maps of N2D+ and para-NH2D) remain independent, so the circularity is partial and does not collapse the entire result.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The claim rests on the assumption that the chosen molecular tracers faithfully sample the same gas parcel and that the external ambipolar-diffusion models correctly capture the microphysics of dust growth and resistivity at the densities and temperatures of L1544.

free parameters (1)
  • dust grain size distribution parameters
    Grain growth parameters are adjusted within the resistivity calculations to reproduce the observed drift velocity.
axioms (1)
  • domain assumption N2D+ and para-NH2D trace identical density and velocity fields within the core interior
    Invoked when comparing velocity centroids of the ion-neutral pair.

pith-pipeline@v0.9.0 · 5920 in / 1367 out tokens · 36935 ms · 2026-05-22T04:05:23.089391+00:00 · methodology

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Works this paper leans on

120 extracted references · 120 canonical work pages

  1. [1]

    2004, in The Dense Interstellar Medium in Galaxies, ed

    Aikawa , Y., Herbst , E., Caselli , P., Roberts , H., & Ohashi , N. 2004, in The Dense Interstellar Medium in Galaxies, ed. S. Pfalzner , C. Kramer , C. Staubmeier , & A. Heithausen , Vol. 91, 461

    work page 2004

  2. [2]

    O., Girart , J

    Alves , F. O., Girart , J. M., Lai , S.-P., Rao , R., & Zhang , Q. 2011, , 726, 63

    work page 2011

  3. [3]

    E., Dapp , W

    Basu , S., Ciolek , G. E., Dapp , W. B., & Wurster , J. 2009, , 14, 483

    work page 2009

  4. [4]

    & Mouschovias , T

    Basu , S. & Mouschovias , T. C. 1995, , 453, 271

    work page 1995

  5. [5]

    T., Padovani , M., Girart , J

    Beltr \'a n , M. T., Padovani , M., Girart , J. M., et al. 2019, , 630, A54

    work page 2019

  6. [6]

    Bonnor , W. B. 1956, MNRAS, 116, 351

    work page 1956

  7. [7]

    2017, , 604, A52

    Bracco , A., Palmeirim , P., Andr \'e , P., et al. 2017, , 604, A52

    work page 2017

  8. [8]

    Bradbury, J., Frostig, R., Hawkins, P., et al. 2018

    work page 2018

  9. [9]

    2012, A & A , 538, A89

    Carter , M., Lazareff , B., Maier , D., et al. 2012, A & A , 538, A89

    work page 2012

  10. [10]

    E., Sipil \"a , O., et al

    Caselli , P., Pineda , J. E., Sipil \"a , O., et al. 2022, , 929, 13

    work page 2022

  11. [11]

    2025, , 703, A77

    Caselli , P., Spezzano , S., Redaelli , E., et al. 2025, , 703, A77

    work page 2025

  12. [12]

    M., Tafalla , M., Dore , L., & Myers , P

    Caselli , P., Walmsley , C. M., Tafalla , M., Dore , L., & Myers , P. C. 1999, , 523, L165

    work page 1999

  13. [13]

    M., Terzieva , R., & Herbst , E

    Caselli , P., Walmsley , C. M., Terzieva , R., & Herbst , E. 1998, , 499, 234

    work page 1998

  14. [14]

    M., Zucconi , A., et al

    Caselli , P., Walmsley , C. M., Zucconi , A., et al. 2002 a , , 565, 331

    work page 2002

  15. [15]

    M., Zucconi , A., et al

    Caselli , P., Walmsley , C. M., Zucconi , A., et al. 2002 b , , 565, 344

    work page 2002

  16. [16]

    2014, in Protostars and Planets VI, ed

    Ceccarelli , C., Caselli , P., Bockel \'e e-Morvan , D., et al. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 859--882

    work page 2014

  17. [17]

    E., Caselli , P., et al

    Chac \'o n-Tanarro , A., Pineda , J. E., Caselli , P., et al. 2019, , 623, A118

    work page 2019

  18. [18]

    2014, , 790, 129

    Chitsazzadeh , S., Di Francesco , J., Schnee , S., et al. 2014, , 790, 129

    work page 2014

  19. [19]

    Ciolek , G. E. & Basu , S. 2000, , 529, 925

    work page 2000

  20. [20]

    P., Tassis , K., & Goldsmith , P

    Clemens , D. P., Tassis , K., & Goldsmith , P. F. 2016, , 833, 176

    work page 2016

  21. [21]

    M., et al

    Crapsi , A., Caselli , P., Walmsley , C. M., et al. 2005, , 619, 379

    work page 2005

  22. [22]

    C., & Tafalla , M

    Crapsi , A., Caselli , P., Walmsley , M. C., & Tafalla , M. 2007, , 470, 221

    work page 2007

  23. [23]

    M., Nutter , D

    Crutcher , R. M., Nutter , D. J., Ward-Thompson , D., & Kirk , J. M. 2004, ApJ, 600, 279

    work page 2004

  24. [24]

    H., Punanova , A., et al

    Daniel , F., Coudert , L. H., Punanova , A., et al. 2016, , 586, L4

    work page 2016

  25. [25]

    A., Caselli , P., et al

    Dartois , E., Noble , J. A., Caselli , P., et al. 2024, Nature Astronomy, 8, 359

    work page 2024

  26. [26]

    DeepMind, Babuschkin, I., Baumli, K., et al. 2020

    work page 2020

  27. [27]

    Di Francesco , J., Andr \'e , P., & Myers , P. C. 2004, , 617, 425

    work page 2004

  28. [28]

    2004, , 413, 1177

    Dore , L., Caselli , P., Beninati , S., et al. 2004, , 413, 1177

    work page 2004

  29. [29]

    Frau , P., Galli , D., & Girart , J. M. 2011, , 535, A44

    work page 2011

  30. [30]

    2026, , 999, 79

    Fukihara, H., Tsukamoto, Y., Hirashita, H., Arzoumanian, D., & Misugi, Y. 2026, , 999, 79

    work page 2026

  31. [31]

    J., Valdivia , V., et al

    Galametz , M., Maury , A. J., Valdivia , V., et al. 2019, , 632, A5

    work page 2019

  32. [32]

    Galli , P. A. B., Loinard , L., Bouy , H., et al. 2019, , 630, A137

    work page 2019

  33. [33]

    2025, , 699, A103

    Giers , K., Spezzano , S., Lin , Y., et al. 2025, , 699, A103

    work page 2025

  34. [34]

    & Mirocha , J

    Ginsburg , A. & Mirocha , J. 2011

    work page 2011

  35. [35]

    2022 a , , 163, 291

    Ginsburg , A., Sokolov , V., de Val-Borro , M., et al. 2022 a , , 163, 291

    work page 2022

  36. [36]

    2022 b , , 163, 291

    Ginsburg , A., Sokolov , V., de Val-Borro , M., et al. 2022 b , , 163, 291

    work page 2022

  37. [37]

    M., Beltr \'a n , M

    Girart , J. M., Beltr \'a n , M. T., Zhang , Q., Rao , R., & Estalella , R. 2009, Science, 324, 1408

    work page 2009

  38. [38]

    M., Rao , R., & Marrone , D

    Girart , J. M., Rao , R., & Marrone , D. P. 2006, Science, 313, 812

    work page 2006

  39. [39]

    A., Barranco , J

    Goodman , A. A., Barranco , J. A., Wilner , D. J., & Heyer , M. H. 1998, ApJ, 504, 223

    work page 1998

  40. [40]

    E., Spezzano , S., et al

    Grassi , T., Pineda , J. E., Spezzano , S., et al. 2026, arXiv e-prints, arXiv:2603.06791

    work page arXiv 2026

  41. [41]

    2010, , 720, 603

    Hezareh , T., Houde , M., McCoey , C., & Li , H.-b. 2010, , 720, 603

    work page 2010

  42. [42]

    2013, , 557, A65

    Hily-Blant , P., Pineau des For \^e ts , G., Faure , A., Le Gal , R., & Padovani , M. 2013, , 557, A65

    work page 2013

  43. [43]

    2010, , 513, A41

    Hily-Blant , P., Walmsley , M., Pineau Des For \^e ts , G., & Flower , D. 2010, , 513, A41

    work page 2010

  44. [44]

    Houde , M., Hull , C. L. H., Plambeck , R. L., Vaillancourt , J. E., & Hildebrand , R. H. 2016, , 820, 38

    work page 2016

  45. [45]

    G., Bastien , P., & Yoshida , H

    Houde , M., Peng , R., Phillips , T. G., Bastien , P., & Yoshida , H. 2000, , 537, 245

    work page 2000

  46. [46]

    E., Hildebrand , R

    Houde , M., Vaillancourt , J. E., Hildebrand , R. H., Chitsazzadeh , S., & Kirby , L. 2009, , 706, 1504

    work page 2009

  47. [47]

    Hull , C. L. H. & Zhang , Q. 2019, Frontiers in Astronomy and Space Sciences, 6, 3

    work page 2019

  48. [48]

    2021, , 913, 85

    Hwang , J., Kim , J., Pattle , K., et al. 2021, , 913, 85

    work page 2021

  49. [49]

    V., Padovani , M., Galli , D., & Caselli , P

    Ivlev , A. V., Padovani , M., Galli , D., & Caselli , P. 2015, , 812, 135

    work page 2015

  50. [50]

    S., Spezzano , S., Caselli , P., Grassi , T., & Haugb lle , T

    Jensen , S. S., Spezzano , S., Caselli , P., Grassi , T., & Haugb lle , T. 2023, , 675, A34

    work page 2023

  51. [51]

    2010, , 711, 655

    Johnstone , D., Rosolowsky , E., Tafalla , M., & Kirk , H. 2010, , 711, 655

    work page 2010

  52. [52]

    2018, , 865, 121

    Kandori , R., Tomisaka , K., Tamura , M., et al. 2018, , 865, 121

    work page 2018

  53. [53]

    L., Evans , II, N

    Kauffmann , J., Bertoldi , F., Bourke , T. L., Evans , II, N. J., & Lee , C. W. 2008, A & A, 487, 993

    work page 2008

  54. [54]

    Kawasaki , Y., Koga , S., & Machida , M. N. 2022, , 515, 2072

    work page 2022

  55. [55]

    & Caselli , P

    Keto , E. & Caselli , P. 2008, , 683, 238

    work page 2008

  56. [56]

    & Caselli , P

    Keto , E. & Caselli , P. 2010, , 402, 1625

    work page 2010

  57. [57]

    W., Tafalla , M., et al

    Kim , S., Lee , C. W., Tafalla , M., et al. 2022, , 940, 112

    work page 2022

  58. [58]

    Kingma, D. P. & Ba, J. 2015, in 3rd International Conference on Learning Representations, ICLR 2015, San Diego, CA, USA, May 7-9, 2015, Conference Track Proceedings, ed. Y. Bengio & Y. LeCun

    work page 2015

  59. [59]

    N., Karska , A., et al

    L \^e , N., Tram , L. N., Karska , A., et al. 2024, , 690, A191

    work page 2024

  60. [60]

    2014, , 562, A83

    Le Gal , R., Hily-Blant , P., Faure , A., et al. 2014, , 562, A83

    work page 2014

  61. [61]

    Le Gouellec , V. J. M., Maury , A. J., Guillet , V., et al. 2020, , 644, A11

    work page 2020

  62. [62]

    2023, , 518, 3326

    Lebreuilly , U., Vallucci-Goy , V., Guillet , V., Lombart , M., & Marchand , P. 2023, , 518, 3326

    work page 2023

  63. [63]

    & Houde , M

    Li , H.-b. & Houde , M. 2008, , 677, 1151

    work page 2008

  64. [64]

    2022, , 665, A131

    Lin , Y., Spezzano , S., Sipil \"a , O., Vasyunin , A., & Caselli , P. 2022, , 665, A131

    work page 2022

  65. [65]

    N., Inutsuka , S.-i., & Matsumoto , T

    Machida , M. N., Inutsuka , S.-i., & Matsumoto , T. 2008, , 676, 1088

    work page 2008

  66. [66]

    A., & Lada , C

    Maret , S., Bergin , E. A., & Lada , C. J. 2006, , 442, 425

    work page 2006

  67. [67]

    Maury , A., Hennebelle , P., & Girart , J. M. 2022, Frontiers in Astronomy and Space Sciences, 9, 949223

    work page 2022

  68. [68]

    McKee , C. F. 1989, , 345, 782

    work page 1989

  69. [69]

    2021, Journal of Molecular Spectroscopy, 377, 111431

    Melosso , M., Bizzocchi , L., Dore , L., et al. 2021, Journal of Molecular Spectroscopy, 377, 111431

    work page 2021

  70. [70]

    1966, , 133, 265

    Mestel , L. 1966, , 133, 265

    work page 1966

  71. [71]

    & Spitzer , Jr., L

    Mestel , L. & Spitzer , Jr., L. 1956, , 116, 503

    work page 1956

  72. [72]

    Mouschovias , T. C. 1979, , 228, 475

    work page 1979

  73. [73]

    Mouschovias , T. C. 1987, in NATO Advanced Study Institute (ASI) Series C, Vol. 210, Physical Processes in Interstellar Clouds, ed. G. E. Morfill & M. Scholer , 491--552

    work page 1987

  74. [74]

    Mouschovias , T. C. 1991, , 373, 169

    work page 1991

  75. [75]

    C., Ciolek , G

    Mouschovias , T. C., Ciolek , G. E., & Morton , S. A. 2011, , 415, 1751

    work page 2011

  76. [76]

    Myers , P. C. 1983, ApJ, 270, 105

    work page 1983

  77. [77]

    C., Basu , S., & Auddy , S

    Myers , P. C., Basu , S., & Auddy , S. 2018, , 868, 51

    work page 2018

  78. [78]

    & Li , Z

    Nakamura , F. & Li , Z. 2008, ApJ, 687, 354

    work page 2008

  79. [79]

    \"O berg , K. I. & Bergin , E. A. 2021, , 893, 1

    work page 2021

  80. [80]

    W., Wilner , D

    Ohashi , N., Lee , S. W., Wilner , D. J., & Hayashi , M. 1999, , 518, L41

    work page 1999

Showing first 80 references.