Relative alignment between dense molecular cores and ambient magnetic field: the synergy of numerical models and observations

Chen, Che-Yu; Behrens, Erica; Washington, J.; Fissel, Laura M.; Friesen, Rachel; Li, Zhi Yun; Pineda, Jaime E.; Ginsburg, Adam; Kirk, Helen; Scibelli, Samantha; Alves, F. O.; Redaelli, E.; Caselli, P.; Punanova, A.; Francesco, James Di; Rosolowsky, Erik; Offner, Stella S. R.; Martín, P. G.; Chacón-Tanarro, A.; Chen, Hope H.H.; Chen, Michael C.Y.; Keown, Jared; Seo, Youngmin; Shirley, Yancy L.; Arce, Héctor G.; Goodman, Alyssa A.; Matzner, Christopher D.; Myers, Philip C.; Singh, Ayushi

doi:10.1093/mnras/staa835

Cited by 11 publications

(3 citation statements)

References 88 publications

(92 reference statements)

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“…Inside dense cores, the magnetic field could influence the transfer of mass and angular momentum from large to small scales and subsequently the formation and evolution of circumstellar disks around protostars (Li et al 2014). Therefore, observational studies of magnetic field structures in comparison with other physical quantities in a large sample of molecular clouds and dense cores are essential to understand the role of the magnetic field in star formation (e.g., Matthews et al 2009;Palmeirim et al 2013;Poidevin et al 2013;Koch et al 2014;Zhang et al 2014;Planck Collaboration et al 2016b;Hull & Zhang 2019;Pattle & Fissel 2019;Chen et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The JCMT BISTRO Survey: Alignment between Outflows and Magnetic Fields in Dense Cores/Clumps

Yen

Koch

Hull

et al. 2021

ApJ

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We compare the directions of molecular outflows of 62 low-mass Class 0 and I protostars in nearby (<450 pc) starforming regions with the mean orientations of the magnetic fields on 0.05-0.5 pc scales in the dense cores/clumps where they are embedded. The magnetic field orientations were measured using the JCMT POL-2 data taken by the BISTRO-1 survey and from the archive. The outflow directions were observed with interferometers in the literature. The observed distribution of the angles between the outflows and the magnetic fields peaks between 15°a nd 35°. After considering projection effects, our results could suggest that the outflows tend to be misaligned with the magnetic fields by 50°±15°in three-dimensional space and are less likely (but not ruled out) randomly

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Section: Introductionmentioning

confidence: 99%

The JCMT BISTRO Survey: Alignment between Outflows and Magnetic Fields in Dense Cores/Clumps

Yen

Koch

Hull

et al. 2021

ApJ

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“…The apparently similar orientations in the large-and core-scale magnetic fields in L 1512, L 1544, and FeSt 1-457 (unless due to a projection effect) suggest that material can accrete onto these cores along magnetic field lines more efficiently than in the case in L 183. Such core formation scenario has been demonstrated by Chen et al (2020) with their turbulent MHD simulations, suggesting that dense cores could accumulate more mass when the core-scale B-fields are aligned with the parsec-scale B-field. However, the L 183 cloud has a total mass of ∼80 M e (Pagani et al 2004), which is considerably larger than the total mass of the L 1544 cloud, estimated to be ∼10 M e (Kim et al 2022).…”

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confidence: 71%

Magnetic Fields of the Starless Core L 1512

Lin,

Lai,

Pattle

et al. 2024

ApJ

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We present JCMT POL-2 850 μm dust polarization observations and Mimir H-band stellar polarization observations toward the starless core L 1512. We detect the highly ordered core-scale magnetic field traced by the POL-2 data, of which the field orientation is consistent with the parsec-scale magnetic fields traced by Planck data, suggesting the large-scale fields thread from the low-density region to the dense core region in this cloud. The surrounding magnetic field traced by the Mimir data shows a wider variation in the field orientation, suggesting there could be a transition of magnetic field morphology at the envelope-scale. L 1512 was suggested to be presumably older than 1.4 Myr in a previous study via time-dependent chemical analysis, hinting that the magnetic field could be strong enough to slow the collapse of L 1512. In this study, we use the Davis–Chandrasekhar–Fermi method to derive a plane-of-sky magnetic field strength (B pos) of 18 ± 7 μG and an observed mass-to-flux ratio (λ obs) of 3.5 ± 2.4, suggesting that L 1512 is magnetically supercritical. However, the absence of significant infall motion and the presence of an oscillating envelope are inconsistent with the magnetically supercritical condition. Using a virial analysis, we suggest the presence of a hitherto hidden line-of-sight magnetic field strength of ∼27 μG with a mass-to-flux ratio (λ tot) of ∼1.6, in which case both magnetic and kinetic pressures are important in supporting the L 1512 core. On the other hand, L 1512 may have just reached supercriticality and will collapse at any time.

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“…Hanawa et al 1993;Gehman et al 1996). Magnetohydrodynamic (MHD) simula-★ E-mail: zwchen@pmo.ac.cn tions and observations of magnetic fields in filaments in the past decades show that magnetic fields play an important role in shaping filaments and regulating the subsequent star formation inside them (Houde et al 2004;Goldsmith et al 2008;Nakamura & Li 2008;Inoue & Inutsuka 2009Heitsch et al 2009;Li et al 2010;Sugitani et al 2011Sugitani et al , 2019Chapman et al 2011;Hennebelle 2013;Soler et al 2013Soler et al , 2016Soler 2019;Matthews et al 2014;Seifried & Walch 2015;Chen & Ostriker 2015;Chen et al 2016Chen et al , 2020Pillai et al 2015Pillai et al , 2020Planck Collaboration et al 2016b,a;Panopoulou et al 2016;Malinen et al 2016;Santos et al 2016;Hoq et al 2017;Zamora-Avilés et al 2018;Mocz & Burkhart 2018;Fissel et al 2019;Kusune et al 2019;Wang et al 2019Wang et al , 2020aSu et al 2020;Körtgen & Soler 2020;Heyer et al 2020;Girichidis 2021;Lee et al 2021;Barreto-Mota et al 2021;Pattle ...…”

Section: Introductionmentioning

confidence: 99%

Strong Magnetic Fields Play Important Role in the Filamentary Infrared Dark Cloud G11.11-0.12

Chen¹,

Sefako²,

Yang³

et al. 2022

Preprint

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We report on the near-infrared polarimetric observations of G11.11-0.12 with the 1.4 m IRSF telescope. The starlight polarization of the background stars reveals the magnetic fields in the envelope of G11.11-0.12, which are consistent in orientation with the magnetic fields obtained from submillimeter dust polarization. The magnetic fields in G11.11-0.12 are perpendicular to the filament in a large column density range, independent of the relative orientations of G11.11-0.12. The field strength on the plane of the sky in G11.11-0.12 has a typical value of 152 ± 17 G. The analyses of the magnetic fields and gas velocity dispersion indicate that the envelope of G11.11-0.12 is supersonic and sub-Alfvénic to trans-Alfvénic. The mass-to-flux ratio in the outer part of the envelope is 1 and slightly increases to 1 closer to the filament. The weights on the relative importance of magnetic fields, turbulence and gravity indicate that gravity has been dominating the dynamical state of G11.11-0.12, with significant contribution from magnetic fields. The field strength increases slower than the gas density from the envelope to the spine of G11.11-0.12, characterized by the relation ∝ 0.2 . The observed strength and orientation of magnetic fields in G11.11-0.12 imply that supersonic gas flow is channelled by sub-Alfvénic magnetic fields and is assembled into filaments perpendicular to the magnetic fields. The formation of low-mass stars is enhanced in the filaments with high column density, in agreement with the excess in numbers of low-mass protostars detected in one of the densest part of G11.11-0.12.

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Relative alignment between dense molecular cores and ambient magnetic field: the synergy of numerical models and observations

Cited by 11 publications

References 88 publications

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

Magnetic Fields of the Starless Core L 1512

Strong Magnetic Fields Play Important Role in the Filamentary Infrared Dark Cloud G11.11-0.12

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