Computer simulations of the formation of massive protostars

Pongracic, H., Chapman, S. J., Davies, J. R., Disney, Michael John, Nelson, A. H. and Whitworth, Anthony Peter ORCID: https://orcid.org/0000-0002-1178-5486 1992. Computer simulations of the formation of massive protostars. Monthly Notices of the Royal Astronomical Society 256 (2) , pp. 291-299. 10.1093/mnras/256.2.291

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Abstract

Attention is given to computer simulations of massive protostar formation which show that in regions of supersonic turbulence such as giant molecular clouds, protostars readily and rapidly condense out of the dense layers which form where two turbulent elements collide at high relative speed. The resulting protostars are rotationally supported disks with well-defined accretion surfaces, masses between 1 and 20 solar masses, diameters in the range 100-400 AU, and densities above 10 exp 12 H2/cu cm, i.e., 10 exp 10 times the initial gas density. The time-scale for formation of these protostellar disks turns out to be shorter than the free-fall time-scale in the initial clouds.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	Oxford University Press
ISSN:	0035-8711
Last Modified:	15 Mar 2024 07:29
URI:	https://orca.cardiff.ac.uk/id/eprint/74374

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