The role of magnetic fields in the stability and fragmentation of filamentary molecular clouds: two case studies at OMC-3 and OMC-4

Li, Pak Shing; Lopez-Rodriguez, Enrique; Soam, Archana; Klein, Richard I.

doi:10.1093/mnras/stac1527

Title: The role of magnetic fields in the stability and fragmentation of filamentary molecular clouds: two case studies at OMC-3 and OMC-4

Journal Article · Fri Jun 03 00:00:00 EDT 2022 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stac1527· OSTI ID:1890088

^[1]; Lopez-Rodriguez, Enrique ^[2];

^[3]; Klein, Richard I. ^[4]

Univ. of California, Berkeley, CA (United States)
Stanford Univ., CA (United States). Kavli Institute for Particle Astrophysics & Cosmology
Indian Institute of Astrophysics, Koramangala, Bengaluru (India)
Univ. of California, Berkeley, CA (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)

We present the stability analysis of two regions, OMC-3 and OMC-4, in the massive and long molecular cloud complex of Orion A. We obtained 214 $$\mu$$m HAWC + /SOFIA polarization data, and we make use of archival data for the column density and C¹⁸O (1–0) emission line. We find clear depolarization in both observed regions and that the polarization fraction is anticorrelated with the column density and the polarization-angle dispersion function. We find that the filamentary cloud and dense clumps in OMC-3 are magnetically supercritical and strongly subvirial. This region should be in the gravitational collapse phase and is consistent with many young stellar objects (YSOs) forming in the region. Our histogram of relative orientation (HRO) analysis shows that the magnetic field is dynamically sub-dominant in the dense gas structures of OMC-3. We present the first polarization map of OMC-4. We find that the observed region is generally magnetically subcritical except for an elongated dense core, which could be a result of projection effect of a filamentary structure aligned close to the line of sight. The relative large velocity dispersion and the unusual positive shape parameters at high column densities in the HROs analysis suggest that our viewing angle may be close to axes of filamentary substructures in OMC-4. The dominating strong magnetic field in OMC-4 is unfavourable for star formation and is consistent with much fewer YSOs than in OMC-3.

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Research Organization:: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA); National Aeronautics and Space Administration (NASA)

Grant/Contract Number:: AC52-07NA27344; NNX17AK39G

OSTI ID:: 1890088

Report Number(s):: LLNL-JRNL-832665; 1049897; TRN: US2310011

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 514, Issue 2; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Title: The role of magnetic fields in the stability and fragmentation of filamentary molecular clouds: two case studies at OMC-3 and OMC-4

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