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Changing structures in galactic star clusters

Schmeja, S., Kumar, M.S.N., Froebrich, Dirk, Klessen, R.S. (2007) Changing structures in galactic star clusters. Proceedings of the International Astronomical Union, 3 (S246). pp. 50-54. ISSN 1743-9213. (doi:10.1017/S1743921308015263) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided) (KAR id:49660)

The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided.
Official URL
http://dx.doi.org/10.1017/S1743921308015263

Abstract

We investigate the structures of embedded and open clusters using statistical methods, in particular the combined parameter $\Q$, which permits to quantify the cluster structure. Star clusters build up from several subclusters evolving from a structured to a more centrally concentrated stage. The evolution is not only a function of time, but also of the mass of the objects. Massive stars are usually centrally concentrated, while lower-mass stars are more widespread, reflecting the effect of mass segregation. Using this method we find that in IC 348 and the Orion Nebula Cluster the spatial distribution of brown dwarfs does not follow the central clustering of stars, giving important clues to their formation mechanism by supporting the ejected embryo scenario.

Item Type: Article
DOI/Identification number: 10.1017/S1743921308015263
Uncontrolled keywords: Methods: statistical, Open clusters and associations: general, Stars: formation
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Divisions > Division of Natural Sciences > Physics and Astronomy
Depositing User: Giles Tarver
Date Deposited: 23 Jul 2015 09:21 UTC
Last Modified: 16 Nov 2021 10:20 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/49660 (The current URI for this page, for reference purposes)
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