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The link between solenoidal turbulence and slow star formation in G0.253+0.016
Federrath, C.; Rathborne, J. M.; Longmore, S. N.; Kruijssen, J. M. D.; Bally, J.; Contreras, Y.; Crocker, R. M.; Garay, G.; Jackson, J. M.; Testi, L.; Walsh, A. J.
AA(Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia ), AB(CSIRO Astronomy and Space Science, P.O. Box 76, Epping NSW, 1710, Australia), AC(Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, United Kingdom), AD(Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, 69120 Heidelberg, Germany), AE(CASA, University of Colorado, 389-UCB, Boulder, CO 80309, USA), AF(Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands), AG(Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia), AH(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile), AI(Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA), AJ(European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching bei München, Germany), AK(International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth WA 6845, Australia)
The Multi-Messenger Astrophysics of the Galactic Centre, Proceedings of the International Astronomical Union, IAU Symposium, Volume 322, pp. 123-128
Publication Date:
Galaxy: centre, ISM: clouds, magnetic fields, stars: formation, turbulence,
Abstract Copyright:
(c) 2017: Copyright © International Astronomical Union 2017
Bibliographic Code:


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 sigmarho /rho 0=1.3+/-0.5 and turbulent Mach number = 11+/-3. Combining these with turbulence simulations to constrain the plasma beta = 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.
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