Probable binary open star clusters in the Galaxy.

dc.contributor.author	Subramaniam, A
dc.contributor.author	Gorti, U
dc.contributor.author	Sagar, R
dc.contributor.author	Bhatt, H. C
dc.date.accessioned	2008-06-30T12:17:42Z
dc.date.available	2008-06-30T12:17:42Z
dc.date.issued	1995-10
dc.identifier.citation	A&A, Vol. 302, No. 1, pp. 86 - 89	en
dc.identifier.issn	0004-6361
dc.identifier.uri	http://hdl.handle.net/2248/2555
dc.description.abstract	The existence of double/binary clusters in the Magellanic Clouds is fairly well established, whereas only one such pair, h + χ Persei, is known in the Galaxy. From the catalogues of open clusters of the Galaxy, we have identified 18 probable pairs of clusters (with known distances), with spatial separations less than 20pc. The tidal disruption timescales for these pairs, due to Galactic differential rotation are calculated, using cluster data where available or by assuming typical values. In some cases, these timescales are larger than the average open cluster lifetime, =~10^8^yr. About 8% of open clusters appear to be members of binary systems, and hence binary cluster systems may not be very uncommon in the Galaxy.	en
dc.format.extent	594565 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	EDP Science	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1995A%26A...302...86S	en
dc.subject	Star clusters	en
dc.subject	Binary clusters	en
dc.subject	Galaxy	en
dc.subject	Galaxy clustering	en
dc.subject	Clustering of Galaxies	en
dc.title	Probable binary open star clusters in the Galaxy.	en
dc.type	Article	en