Cooling behind mildly supersonic shocks in molecular clouds

Whitworth, Anthony Peter ORCID: https://orcid.org/0000-0002-1178-5486 and Clarke, C. J. 1997. Cooling behind mildly supersonic shocks in molecular clouds. Monthly Notices of the Royal Astronomical Society 291 (3) , pp. 578-584. 10.1093/mnras/291.3.578

Full text not available from this repository.

Abstract

Collisions between stable, thermally supported gas clumps produce shock-compressed layers. However, these layers then undergo gravitational fragmentation only if the gas cools — on a dynamical time-scale or faster — to below its pre-shock temperature. Here we present an approximate analytic treatment of post-shock cooling which demonstrates that, under the conditions prevailing in molecular clouds, where the typical collision speeds are ~ 1 km s−1, cooling by dust is likely to be the dominant cooling mechanism, and is sufficiently fast to satisfy this requirement. Cooling by CO appears to be of secondary importance.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Schools > Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	Oxford University Press
ISSN:	0035-8711
Last Modified:	28 Oct 2022 09:03
URI:	https://orca.cardiff.ac.uk/id/eprint/73095

Citation Data

Cited 15 times in Scopus. View in Scopus. Powered By Scopus® Data

Actions (repository staff only)

Edit Item