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The link between solenoidal turbulence and slow star formation in G0.253+0.016

Published online by Cambridge University Press:  09 February 2017

C. Federrath Open the ORCID record for C. Federrath [Opens in a new window] ,
J. M. Rathborne ,
S. N. Longmore ,
J. M. D. Kruijssen ,
J. Bally ,
Y. Contreras ,
R. M. Crocker ,
G. Garay ,
J. M. Jackson  and
L. Testi
...Show all authors
C. Federrath
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia email: christoph.federrath@anu.edu.au
J. M. Rathborne
Affiliation:
CSIRO Astronomy and Space Science, P.O. Box 76, Epping NSW, 1710, Australia
S. N. Longmore
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, United Kingdom
J. M. D. Kruijssen
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, 69120 Heidelberg, Germany Max-Planck Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
J. Bally
Affiliation:
CASA, University of Colorado, 389-UCB, Boulder, CO 80309, USA
Y. Contreras
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands
R. M. Crocker
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia email: christoph.federrath@anu.edu.au
G. Garay
Affiliation:
Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
J. M. Jackson
Affiliation:
Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA
L. Testi
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching bei München, Germany INAF-Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy Excellence Cluster Universe, Boltzmannstraße 2, D-85748, Garching, Germany
A. J. Walsh
Affiliation:
International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth WA 6845, Australia
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Abstract

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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.

Keywords

Galaxy: centreISM: cloudsmagnetic fieldsstars: formationturbulence

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