Star formation in transient molecular clouds

Clark, Paul ORCID: https://orcid.org/0000-0002-4834-043X and Bonnell, I. A. 2004. Star formation in transient molecular clouds. Monthly Notices of the Royal Astronomical Society 347 (2) , L36-L40. 10.1111/j.1365-2966.2004.07377.x

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Abstract

We present the results of a numerical simulation in which star formation proceeds from an initially unbound molecular cloud core. The turbulent motions, which dominate the dynamics, dissipate in shocks leaving a quiescent region which becomes gravitationally bound and collapses to form a small multiple system. Meanwhile, the bulk of the cloud escapes due to its initial supersonic velocities. In this simulation, the process naturally results in a star formation efficiency of ∼50 per cent. The mass involved in star formation depends on the gas fraction that dissipates sufficient kinetic energy in shocks. Thus, clouds with larger turbulent motions will result in lower star formation efficiencies. This implies that globally unbound, and therefore transient giant molecular clouds (GMCs), can account for the low efficiency of star formation observed in our Galaxy without recourse to magnetic fields or feedback processes. Observations of the dynamic stability in molecular regions suggest that GMCs may not be self-gravitating, supporting the ideas presented in this letter.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	stars: formation; ISM: clouds; ISM: kinematics and dynamics; ISM: structure
Publisher:	Oxford University Press
ISSN:	0035-8711
Last Modified:	25 Oct 2022 09:45
URI:	https://orca.cardiff.ac.uk/id/eprint/59913

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