Curtin University Homepage
  • Library
  • Help
    • Admin

    espace - Curtin’s institutional repository

    JavaScript is disabled for your browser. Some features of this site may not work without it.
    View Item 
    • espace Home
    • espace
    • Curtin Research Publications
    • View Item
    • espace Home
    • espace
    • Curtin Research Publications
    • View Item

    The Link Between Turbulence, Magnetic Fields, Filaments, And Star Formation In The Central Molecular Zone Cloud G0.253+0.016

    261299.pdf (1.617Mb)
    Access Status
    Open access
    Authors
    Federrath, C.
    Rathborne, J.
    Longmore, S.
    Kruijssen, J.
    Bally, J.
    Contreras, Y.
    Crocker, R.
    Garay, G.
    Jackson, J.
    Testi, L.
    Walsh, Andrew
    Date
    2016
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Federrath, C. and Rathborne, J. and Longmore, S. and Kruijssen, J. and Bally, J. and Contreras, Y. and Crocker, R. et al. 2016. The Link Between Turbulence, Magnetic Fields, Filaments, And Star Formation In The Central Molecular Zone Cloud G0.253+0.016. Astrophysical Journal. 832 (2).
    Source Title
    Astrophysical Journal
    DOI
    10.3847/0004-637X/832/2/143
    ISSN
    0004-637X
    School
    Curtin Institute of Radio Astronomy (Physics)
    Remarks

    Copyright © 2016 The American Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/63153
    Collection
    • Curtin Research Publications
    Abstract

    © 2016. The American Astronomical Society. All rights reserved.Star formation is primarily controlled by the interplay between gravity, turbulence, and magnetic fields. However, the turbulence and magnetic fields in molecular clouds near the Galactic center may differ substantially compared to spiral-arm clouds. Here we determine the physical parameters of the central molecular zone (CMZ) cloud G0.253+0.016, its turbulence, magnetic field, and filamentary structure. Using column density maps based on dust-continuum emission observations with ALMA+Herschel, we identify filaments and show that at least one dense core is located along them. We measure the filament width and the sonic scale of the turbulence, and find Wfil ˜ ?sonic. A strong velocity gradient is seen in the HNCO intensity-weighted velocity maps obtained with ALMA+Mopra. The gradient is likely caused by large-scale shearing of G0.253+0.016, producing a wide double-peaked velocity probability distribution function (PDF). After subtracting the gradient to isolate the turbulent motions, we find a nearly Gaussian velocity PDF typical for turbulence. We measure the total and turbulent velocity dispersion, 8.8 ± 0.2 km s-1 and 3.9 ± 0.1 km s-1, respectively. Using magnetohydrodynamical turbulence simulations, we find that G0.253+0.016's turbulent magnetic Bturb = 130 ± 50 µG is only ? 1/10 only of the ordered field component. Combining these measurements, we reconstruct the dominant turbulence driving mode in G0.253+0.016 and find a driving parameter of b = 0.22 ± 0.12, indicating solenoidal (divergence-free) driving. We compare this to spiral-arm clouds, which typically have a significant compressive (curl-free) driving component (b > 0.4). Motivated by previous reports of strong shearing motions in the CMZ, we speculate that shear causes the solenoidal driving in G0.253+0.016 and show that this reduces the star-formation rate by a factor of 6.9 compared to typical nearby clouds.

    Related items

    Showing items related by title, author, creator and subject.

    • The link between solenoidal turbulence and slow star formation in G0.253+0.016
      Federrath, C.; Rathborne, J.; Longmore, S.; Kruijssen, J.; Bally, J.; Contreras, Y.; Crocker, R.; Garay, G.; Jackson, J.; Testi, L.; Walsh, Andrew (2016)
      Star formation in the Galactic disc is primarily controlled by gravity, turbulence, and magnetic fields. It is not clear that this also applies to star formation near the Galactic Centre. Here we determine the turbulence ...
    • Absorption filaments toward the massive clump G0.253+0.016
      Bally, J.; Rathborne, J.; Longmore, S.; Jackson, J.; Alves, J.; Bressert, E.; Contreras, Y.; Foster, J.; Garay, G.; Ginsburg, A.; Johnston, K.; Kruijssen, J.; Testi, L.; Walsh, Andrew (2014)
      ALMA HCO+ observations of the infrared dark cloud G0.253+0.016 located in the central molecular zone of the Galaxy are presented. The 89 GHz emission is area-filling, optically thick, and sub-thermally excited. Two types ...
    • Absorption filaments toward the massive clump G0.253+0.016
      Bally, J.; Rathborne, J.; Longmore, S.; Jackson, J.; Alves, J.; Bressert, E.; Contreras, Y.; Foster, J.; Garay, G.; Ginsburg, A.; Johnston, K.; Kruijssen, J.; Testi, L.; Walsh, Andrew (2014)
      ALMA HCO+ observations of the infrared dark cloud G0.253+0.016 located in the central molecular zone of the Galaxy are presented. The 89 GHz emission is area-filling, optically thick, and sub-thermally excited. Two types ...
    Advanced search

    Browse

    Communities & CollectionsIssue DateAuthorTitleSubjectDocument TypeThis CollectionIssue DateAuthorTitleSubjectDocument Type

    My Account

    Admin

    Statistics

    Most Popular ItemsStatistics by CountryMost Popular Authors

    Follow Curtin

    • 
    • 
    • 
    • 
    • 

    CRICOS Provider Code: 00301JABN: 99 143 842 569TEQSA: PRV12158

    Copyright | Disclaimer | Privacy statement | Accessibility

    Curtin would like to pay respect to the Aboriginal and Torres Strait Islander members of our community by acknowledging the traditional owners of the land on which the Perth campus is located, the Whadjuk people of the Nyungar Nation; and on our Kalgoorlie campus, the Wongutha people of the North-Eastern Goldfields.