The formation of OB subgroups

Chapman, S. J., Bhattal, A. S., Disney, Michael John, Turner, J. A. and Whitworth, Anthony Peter ORCID: https://orcid.org/0000-0002-1178-5486 1994. The formation of OB subgroups. Presented at: Proceedings of the First UNAM-CRAY Supercomputing Workshop, 'Numerical Simulations in Astrophysics : Modelling the Dynamics of the Universe' ,, Mexico City, México, 26-30 July 1993. Published in: Franco, José ed. Numerical Simulations in Astrophysics: Proceedings of the First UNAM-CRAY Supercomputing Workshop, 'Numerical Simulations in Astrophysics : Modelling the Dynamics of the Universe' Held in Mexico City, México, July 26-30, 1993. Cambridge, UK: Cambridge University Press, pp. 206-224.

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Abstract

The authors analyze the gravitational stability of shocked interstellar gas layers, and show that, irrespective of the mechanism that generates them, (i) they first fragment gravitationally when the hydrogen column density reaches a value ≡6×1021cm-2; and (ii) the resulting fragments are massive, ≥7 Msun. These results may help to explain Larson's relations between the masses and sizes of clumps in GMCs, and why massive star formation tends to be self-propagating. The authors present a numerical simulation which confirms this analysis and produces a cluster of ≡50 protostars resembling a nascent OB Association. The protostars are all massive, ≥5 Msun, and most are in binary or multiple systems.

Item Type:	Conference or Workshop Item (Paper)
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	Star Formation: Gas Dynamics, Star Formation: OB Associations
Publisher:	Cambridge University Press
ISBN:	9780521462389
Last Modified:	15 Nov 2022 12:25
URI:	https://orca.cardiff.ac.uk/id/eprint/74199

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