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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5996
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dc.contributor.authorBhavya, B-
dc.contributor.authorSubramaniam, A-
dc.contributor.authorKuriakose, V. C-
dc.date.accessioned2013-02-18T11:17:29Z-
dc.date.available2013-02-18T11:17:29Z-
dc.date.issued2012-
dc.identifier.citationASI Conference Series, Vol. 4, pp. 121-124en
dc.identifier.isbn978-81-922926-2-5-
dc.identifier.urihttp://hdl.handle.net/2248/5996-
dc.descriptionOpen Accessen
dc.description.abstractYoung Open Clusters have always been a platform for the star formation studies. It was assumed that all members in the cluster are coeval, on the other hand, recent studies show the presence of an age range among the members of young open clusters. Presence of pre-main sequence (PMS) stars are identified by combining optical and near-IR data for 13 young clusters. Age-wise and mass-wise distribution of PMS stars are analysed to study how star formation proceeded in the clusters. In all the clusters we studied, we find an age range among the PMS stars and the duration of star formation is found to be similar to the cluster age.en
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.relation.urihttp://www.ncra.tifr.res.in:8081/~basi/ASICS_4/Abstracts/bhavya.htmlen
dc.rights© Astronomical Society of Indiaen
dc.subjectStarsen
dc.subjectFormation -- starsen
dc.subjectPre-main sequence -- (Galaxy)en
dc.subjectOpen clusters and associations generalen
dc.titleDuration of star formation in young open clustersen
dc.typeArticleen
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