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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4082
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dc.contributor.authorRajamohan, R-
dc.date.accessioned2008-12-16T14:45:13Z-
dc.date.available2008-12-16T14:45:13Z-
dc.date.issued1978-09-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Vol. 184, pp. 743 - 753en
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2248/4082-
dc.descriptionOpen Access-
dc.description.abstractAnalysis 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.isoenen
dc.publisherRoyal Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/1978MNRAS.184..743Ren
dc.rights©Royal Astronomical Society-
dc.subjectGalactic Clustersen
dc.subjectMain Sequence Starsen
dc.subjectStellar Rotationen
dc.subjectAngular Momentumen
dc.subjectAstronomical Spectroscopyen
dc.subjectBinary Starsen
dc.subjectVelocity Distributionen
dc.titleStellar rotation on the zero age main sequenceen
dc.typeArticleen
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