Stellar rotation on the zero age main sequence

dc.contributor.author	Rajamohan, R
dc.date.accessioned	2008-12-16T14:45:13Z
dc.date.available	2008-12-16T14:45:13Z
dc.date.issued	1978-09
dc.identifier.citation	Monthly Notices of the Royal Astronomical Society, Vol. 184, pp. 743 - 753	en
dc.identifier.issn	0035-8711
dc.identifier.uri	http://hdl.handle.net/2248/4082
dc.description	Open Access
dc.description.abstract	Analysis of rotational velocities of unevolved members in clusters indicates that for a given mass the dispersion in the true rotational velocities is small for normal, single main-sequence stars. The envelope of highest rotation of rich clusters and associations is utilized to derive the rotational velocities on the zero age main sequence. It is suggested (1) that the zero age main-sequence rotation curve defines the star's stability against fission and (2) that the frequency of spectroscopic binaries in a cluster is determined by the total angular momentum available to the gas cloud before fragmentation.	en
dc.language.iso	en	en
dc.publisher	Royal Astronomical Society	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1978MNRAS.184..743R	en
dc.rights	©Royal Astronomical Society
dc.subject	Galactic Clusters	en
dc.subject	Main Sequence Stars	en
dc.subject	Stellar Rotation	en
dc.subject	Angular Momentum	en
dc.subject	Astronomical Spectroscopy	en
dc.subject	Binary Stars	en
dc.subject	Velocity Distribution	en
dc.title	Stellar rotation on the zero age main sequence	en
dc.type	Article	en