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

C. Federrath; J. M. Rathborne; S. N. Longmore; J. M.D. Kruijssen; J. Bally; Y. Contreras; R. M. Crocker; G. Garay; J. M. Jackson; L. Testi; A. J. Walsh

doi:10.1017/S1743921316012357

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

C. Federrath, J. M. Rathborne, S. N. Longmore, J. M.D. Kruijssen, J. Bally, Y. Contreras, R. M. Crocker, G. Garay, J. M. Jackson, L. Testi, A. J. Walsh

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6 Citations (Scopus)

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/ρ0=1.3±0.5 and turbulent Mach number = 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.

Original language	English
Pages (from-to)	123-128
Number of pages	6
Journal	Proceedings of the International Astronomical Union
Volume	11
DOIs	https://doi.org/10.1017/S1743921316012357
Publication status	Published - 2016

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@article{ea2feef144b94b81a1422ae0fd2a2eef,

title = "The link between solenoidal turbulence and slow star formation in G0.253+0.016",

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/ρ0=1.3±0.5 and turbulent Mach number = 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: centre, ISM: clouds, magnetic fields, stars: formation, turbulence",

author = "C. Federrath and Rathborne, {J. M.} and Longmore, {S. N.} and Kruijssen, {J. M.D.} and J. Bally and Y. Contreras and Crocker, {R. M.} and G. Garay and Jackson, {J. M.} and L. Testi and Walsh, {A. J.}",

note = "Publisher Copyright: {\textcopyright} Copyright International Astronomical Union 2017.",

year = "2016",

doi = "10.1017/S1743921316012357",

language = "English",

volume = "11",

pages = "123--128",

journal = "Proceedings of the International Astronomical Union",

issn = "1743-9213",

publisher = "Cambridge University Press",

}

TY - JOUR

T1 - The link between solenoidal turbulence and slow star formation in G0.253+0.016

AU - Federrath, C.

AU - Rathborne, J. M.

AU - Longmore, S. N.

AU - Kruijssen, J. M.D.

AU - Bally, J.

AU - Contreras, Y.

AU - Crocker, R. M.

AU - Garay, G.

AU - Jackson, J. M.

AU - Testi, L.

AU - Walsh, A. J.

N1 - Publisher Copyright: © Copyright International Astronomical Union 2017.

PY - 2016

Y1 - 2016

N2 - 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/ρ0=1.3±0.5 and turbulent Mach number = 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.

AB - 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/ρ0=1.3±0.5 and turbulent Mach number = 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.

KW - Galaxy: centre

KW - ISM: clouds

KW - magnetic fields

KW - stars: formation

KW - turbulence

UR - http://www.scopus.com/inward/record.url?scp=85012254484&partnerID=8YFLogxK

U2 - 10.1017/S1743921316012357

DO - 10.1017/S1743921316012357

M3 - Article

SN - 1743-9213

VL - 11

SP - 123

EP - 128

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

ER -

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

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