The turbulent ISM and the stellar IMF

Clark, Paul ORCID: https://orcid.org/0000-0002-4834-043X and Klessen, R.S. 2008. The turbulent ISM and the stellar IMF. Astronomische Nachrichten 329 (9-10) , pp. 960-963. 10.1002/asna.200811050

Full text not available from this repository.

Abstract

In this contribution, we focus on the role that turbulence can play in setting the initial mass function (IMF) of stars. Two theories are contrasted. In the first, the so-called ‘turbulent’ fragmentation theory, the turbulence is directly responsible for breaking up the cloud into ‘cores’ which go on to form either a single star or a small N system. In such a picture, the IMF is primordial, since the mass reservoir form the young protostellar system is assumed to be set by the mass of the natal core. In the alternative picture, ‘competitive accretion’, the final mass of a protostar is determined by its position in the potential well of the cluster. As such the IMF is determined through gravitational dynamics rather than turbulence. We discuss the observation motivation for each of these cases.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	ISM: clouds; ISM: kinematics and dynamics; ISM: structure; stars: formation
Publisher:	Wiley
ISSN:	0004-6337
Last Modified:	25 Oct 2022 09:44
URI:	https://orca.cardiff.ac.uk/id/eprint/59853

Citation Data

Cited 1 time in Scopus. View in Scopus. Powered By Scopus® Data

Actions (repository staff only)

Edit Item