dc.contributor.author Federrath, C. dc.contributor.author Rathborne, J. dc.contributor.author Longmore, S. dc.contributor.author Kruijssen, J. dc.contributor.author Bally, J. dc.contributor.author Contreras, Y. dc.contributor.author Crocker, R. dc.contributor.author Garay, G. dc.contributor.author Jackson, J. dc.contributor.author Testi, L. dc.contributor.author Walsh, Andrew dc.date.accessioned 2017-03-15T22:27:43Z dc.date.available 2017-03-15T22:27:43Z dc.date.created 2017-03-14T06:55:53Z dc.date.issued 2016 dc.identifier.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 solenoidal turbulence and slow star formation in G0.253+0.016, in Crocker, R. and Longmore, S. and Bicknell, G. (eds), Proceedings of the International Astronomical Union Symposia and Colloquia: The Multi-Messenger Astrophysics of the Galactic Centre, Jul 18-20 2016, 11 (S322), pp. 123-128. Palm Cove, Australia: IAU. dc.identifier.uri http://hdl.handle.net/20.500.11937/50759 dc.identifier.doi 10.1017/S1743921316012357 dc.description.abstract 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 and star formation in the CMZ cloud G0.253+0.016. Using maps of 3 mm dust emission and HNCO intensity-weighted velocity obtained with ALMA, we measure the volume-density variance σρ /ρ 0=1.3±0.5 and turbulent Mach number $\mathcal{M}$ = 11±3. Combining these with turbulence simulations to constrain the plasma β = 0.34±0.35, we reconstruct the turbulence driving parameter b=0.22±0.12 in G0.253+0.016. This low value of b indicates solenoidal (divergence-free) driving of the turbulence in G0.253+0.016. By contrast, typical clouds in the Milky Way disc and spiral arms have a significant compressive (curl-free) driving component (b > 0.4). We speculate that shear causes the solenoidal driving in G0.253+0.016 and show that this may reduce the star formation rate by a factor of 7 compared to nearby clouds. dc.title The link between solenoidal turbulence and slow star formation in G0.253+0.016 dc.type Conference Paper dcterms.source.volume 11 dcterms.source.startPage 123 dcterms.source.endPage 128 dcterms.source.issn 1743-9213 dcterms.source.title Proceedings of the International Astronomical Union dcterms.source.series Proceedings of the International Astronomical Union curtin.department Curtin Institute of Radio Astronomy (Physics) curtin.accessStatus Open access
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